George  Davidson 
1925-1911 


FRONTISPIECE.— Silver  print  of  the  Total  Solar  Eclipse  of  December, 
1889,  from  negatives  by  S.  W.  BURNHAM. 


/ 


/  //  •>,..-.  &&-<*-<  •*- fa-  V 


REPORTS  ON  rffiE  OBSERVATIONS 


TOTAL  ECLIPSE  OF  THE  SUN, 


DECEMBER  21-22,  1889, 


AND   OF   THE 


TOTAL  ECLIPSE  OF  THE  MOON,  JULY  22, 


TO   WHICH    IS  ADDED 


A  CATALOOUE  OK  THE  LIBRARY, 

PUBLISHED  BY  THE  LICK  OBSERVATORY. 


Printed  by  authority  of  the  Regents  of  the  University  of  California. 


SACRAMENTO: 

STATE    OFFICE,    :    :    :    A.    J.   JOHNSTON,    SUPT.    STATE    PRINTING. 

1891. 


f 


The  Expedition  to  observe  the  Total  Eclipse  of  the  Sun  of  December 
21-22,  1889,  was  sent  from  the  Lick  Observatory  at  the  cost  of 
Hon.  Charles  F.  Crocker,  Regent  of  the  University  of  California. 


L:r 

TABLE  OE  CONTENTS. 


TOTAL  SOLAR  ECLIPSE  OF  DECEMBER,  1889.  * 

PAGE. 

I.  Introduction,  by  EDWARD  8.  HOLDEN .. 1 

Acknowledgments _ 2 

Examination  of  the  eclipse  negatives . 8 

Dimensions  of  the  corona . 3 

Negative  of  the  total  phase,  by  Monsieur  L'HOTE 4 

Photographic  photometry  of  the  corona 4 

Observations  of  the  Eclipse  of  January,  1889_._ _ 8 

Observations  of  the  Eclipse  of  December,  1889 9 

Photometric  measures  of  the  December  eclipse  plates 9 

Total  light  of  the  corona 11 

The  standardized  plates 11 

Test-plates . 12 

Photometric  results. ._ 14 

Extension  of  the  outer  corona. 17 

Conclusion 20 

II.  Report  of  S.  W.  BURNHAM  and  J.  M.  SCHAEBERLE _  22 

The  6^-inch  CLARK  equatorial 23 

The  DALLMEYER  photographic  telescope _ 25 

The  18-inch  reflector 27 

Observation  of  contacts 29 

The  eclipse  negatives 31 

General  features  of  the  corona 37 

Serrations  and  protuberances  visible  on  Negative  No.  2 39 

Orientation  of  the  prints 40 

Photographic  prints .._ 40 

Photography  in  the  tropics 42 

The  Eclipse  parties  at  Isles  du  Salut 44 

Conclusion 45 

III.  A  mechanical  theory  of  the  solar  corona,  by  J.  M.  SCHAEBERLE 47 

IV.  Report  of  E.  E.BARNARD 103 


TOTAL    LUNAR   ECLIPSE    OF    JULY,  1888. 

Introduction - 108 

Observations  with  the  36-inch  telescope,  by  EDWARD  S.  HOLDEN  and 

J.  M.  SCHAEBERLE 109 

Conclusions - 112 

Naked-eye  drawings,  by  EDWARD  S.  HOLDEN — 113 

Spectroscopic  observations,  by  J.  E.  KEELER 115 

Observations  and  photographs,  by  E.  E.  BARNARD 117 

Contacts  observed,  by  CHARLES  B.  HILL 121 

Catalogue  of  the  Library  of  the  Lick  Observatory.    Prepared  by  EDWARD 

S.  HOLDEN . - -  1* 

Works  issued  by  the  Lick  Observatory 122* 


LIST  OF  ILLUSTRATIONS. 


I'i.vn: 


I'l.ATK  II. 


Silver  print  of  the  Total  Solar  Eclipse  of  December,  1889; 

from  negatives  by  S.  W.  BUBNH  AM  ...  -  -  Frontispiece. 

NOTE.— The  top  of  the  page  is  east,  the  right  hand  edge  is 
north.  Some  of  the  copies  of  the  Report  contain  a  frontis- 
piece in  which  the  original  is  enlarged  about  two  diameters. 


Public  Square,  Cayenne  ;  from  a  negative  by  S.  W.  BURN- 
HAM;  to  face  page  ...........  -------------  -,  ........  --- 

PLATE      III.    The  6-inch  equatorial;  to  face  page  ----- 

FIGURE       1.     Lines  of  equal  density  in  one  of  the  Eclipse  Negatives  (in 

the  text)  ____  .........  ...  .....  __________  :  ------------  37 

PLATE  IV.  Silver  print  of  the  Total  Solar  Eclipse  of  December,  1889; 
from  negative  made  with  the  U.  S.  Naval  Observatory 
camera,  by  J.  M.  SCHAEBERLE;  to  face  page  ----------  37 

NOTE.—  The  top  of  the  page  is  east,  the  right  hand  edge  is 
north. 

Silver  print  of  the  Total  Solar  Eclipse  of  December,  1889; 
from  a  negative  by  J.  M.  SCHAEBERLE,  made  with  a 
reflector  constructed  by  himself;  to  face  page  _______  .  39 

NOTE.—  The  top  of  the  page  is  west,  the  right  hand  edge  is 
north. 


PLATE       V. 


PLATE  VI. 
PLATE  VII. 
PLATE  VIII. 

PLATE  IX. 
PLATE  A. 
PLATE  B. 


Model  illustrating  a  Mechanical  Theory  of  the  Solar 

Corona,  by  J.  M.  SCHAEBERLE;  to  face  page  .......  ...  47 

Models  illustrating  the  method  of  formation  of  the  polar 

rays,  by  J.  M.  SCHAEBERLE;  to  face  page  ____  .....  ____  47 

Diagram  illustrating  variation  in  the  curvature  and  posi- 
tion of  a  single  streamer  in  projection,  by  J.  M.  SCHAE- 
BERLE; to  face  page  .............  ______________  .....  _  56 

Diagrams  of  the  actinic  intensity  of  the  Solar  Coronas  of 
January  and  December,  1889;  deduced  by  E.  E.  BAR- 
NARD; to  face  page  ______________  ........  _  ...........  _.  108 

Diagrams  to  illustrate  the  distribution  of  light  at  the 
Lunar  Eclipse  of  July,  1888,  by  J.  M.  SCHAEBERLE  ;  to 
face  page  .............  _  .............  ________  ........  ..  ill 

Naked-eye  sketches  of  the  Lunar  Eclipse  of  July,  1888, 

by  E.  S.  HOLDEN  and  J.  E.  KEELER;  to  face  page  _____  114 


N.  B.— All  of  the  prints  of  the  Solar  Eclipse  are  made  from  unretonched  negatives, 
unless  otherwise  expressly  stated  in  the  text. 


TOTAL  SOLAR  ECLIPSE  OF  DECEMBER,  1889. 


I.    INTRODUCTION. 

By  EDWABD  S.  HOLDEN. 


The  observations  of  the  total  solar  eclipse  of  January  1, 1889, 
made  by  the  astronomers  of  the  Lick  Observatory,  and  by  many 
other  observers,  are  printed  in  a  special  report,  which  has  been 
distributed  during  the  past  year.* 

The  results  derived  from  the  photographs  of  this  eclipse,  espe- 
cially from  those  taken  by  Mr.  BARNARD,  of  the  Lick  Observa- 
tory, and  by  Messrs.  LOWDEN  and  IRELAND,  of  the  Amateur 
Photographic  Association  of  the  Pacific  Coast,  were  interesting 
and  important.  It  was  therefore  desired  to  take  advantage  of 
the  photographic  experience  then  gained,  and  to  observe  the 
total  eclipse  of  December  twenty-first  in  the  same  manner. 

It  was,  however,  found  to  be  impossible  for  the  Lick  Observ- 
atory to  fit  out  an  expedition  from  the  funds  annually  allotted 
to  it,  and  the  plan  of  observing  this  eclipse  had  been  reluct- 
antly abandoned,  when  Hon.  CHARLES  F.  CROCKER,  a  Regent 
of  the  University,  generously  offered  to  bear  the  entire  cost 
of  an  eclipse  expedition  to  South  America.  Accordingly,  the 
Regents  of  the  University  authorized  the  absence  of  Messrs. 
BURNHAM  and  SCHAEBERLE,  and  the  loan  of  the  necessary  in- 
struments from  the  Observatory;  and  I  was  instructed  to  pre- 
pare a  programme  of  observations  to  be  made,  etc. 

This  was  done  after  consultation  with  all  the  astronomers  of 
the  Observatory,  and  delivered  to  the  observers  in  July,  1889. 

The  principal  points  of  the  programme  were  also  communi- 
cated to  the  Superintendent  of  the  U.  S.  Naval  Observatory, 
and  to  the  Secretary  of  the  Eclipse  Committee  of  the  Royal 
Astronomical  Society,  and  they  are  sufficiently  indicated  in 

*  Reports  on  the  Observations  of  the  Total  Eclipse  of  the  Sun  of  January  1, 
1889,  published  by  the  Lick  Observatory.  Printed  by  authority  of  the  Regents 
of  the  University  of  California.  Sacramento,  1889.  8vo,  pp.  xii,  210. 


Solar  Eclipse  of  December,  1889. 


the  joint  report  of  Messrs.  BURNHAM  and  SCHAEBERLE,  follow- 
ing. 

ACKNOWLEDGMENTS. 

The  acknowledgments  of  the  Observatory  are  due,  and  are 
gratefully  returned,  not  only  to  Hon.  C.  F.  CROCKER,  without 
whose  aid  the  expedition  would  have  been  impossible,  but  also 
to  Captain  R.  L.  PHYTHIAN,  U.  S.  Navy,  Superintendent  of  the 
Naval  Observatory  at  Washington,  to  whose  interest  in  the  ex- 
pedition we  owe  the  loan  of  the  six-inch  DALLMEYER  camera 
used  by  Mr.  SCHAEBERLE;,  as  well  as  to  F.  G.  BLINN,  Esq.,  of 
Oakland,  who  put  the  entire  equipment  of  his  private  observa- 
tory at  our  disposition.  From  among  his  portable  instruments 
we  selected  a  sextant  which  was  used  at  the  station.  The 
Observatory  is  also  indebted  to  C.  H.  ROCKWELL,.  Esq.,  who 
joined  the  expedition  as  a  volunteer  observer,  and  who  took 
part  in  the  observations;  and  to  Monsieur  HENRI  L'HOTE,  of  the 
Administration  of  the  Military  Hospital  at  Cayenne,  who 
furnished  the  Observatory  with  a  negative  taken  by  himself 
with  a  small  camera. 

The  operations  of  the  expedition  were  also  greatly  facilitated 
by  the  kindness  of  the  following  gentlemen,  who  interested 
themselves  in  our  behalf,  namely: 

Hon.  JAMES  G.  BLAINE,  Secretary  of  State,  Washington, 

Hon.  WILLIAM  WINDOM,  Secretary  of  the  Treasury,  Washing- 
ton, 

Monsieur  THEODORE  ROUSTAN,  Minister  of  France  to  the 
United  States,  Washington, 

Admiral  E.  MoticHEz,  Director  of  the  National  Observatory, 
Paris, 

Monsieur  GERVILLE  REACHE,  Governor  of  French  Guiana, 
Cayenne, 

Mr.  WACOGNE,  American  Consul  at  Cayenne, 

Hon.  T.  GUY  PHELPS,  Collector  of  Customs  at  San  Francisco, 
and  Chairman  of  the  Committee  of  the  Regents  on  the  Lick 
Observatory. 

We  have  also  to  thank  the  Secretary  of  the  Eclipse  Com- 
mittee of  the  R.  A.  S.,  H.  H.  TURNER,  Esq.,  for  information  as 
to  the  plans  of  this  committee. 

The  Rev.  Father  PERRY,  S.  J.,  who  died  at  his  post  immedi- 


Introduction  by  Mr.  H olden. 


ately  after  the  completion  of  his  work  at  the  British  Eclipse 
Station  in  South  America  (Salute  I.),  had  also  been  in  constant 
communication  with  the  Lick  Observatory,  and  our  cooperation 
was  complete.  It  may  be  permitted  to  his  fellow  astronomers 
to  signify  their  esteem  and  respect  for  his  high  character  and 
eminent  services,  and  to  envy  the  manner  of  his  death,  coming 
as  it  did  after  a  duty  performed  to  the  utmost,  and  after  a  long 
life  devoted  to  his  chosen  science. 


EXAMINATION   OF   THE   ECLIPSE   NEGATIVES. 

When  the  negatives  of  the  eclipse  of  January,  1889,  were 
returned  to  the  Observatory,  I  made  a  careful  study  of  them 
in  certain  respects,  the  results  of  which  are  printed  in  the 
report  of  that  eclipse.  I  have  made  a  similar  study  of  the 
negatives  of  the  December  eclipse,  and  give  the  principal 
results  in  what  follows: 

DIMENSIONS  OF  THE  CORONA. 

There  are  four  main  wings  to  the  corona.  For  the  purpose 
of  describing  them,  I  have  used  the  following  nomenclature: 

I  is  the  north  edge  of  the  north  wing  on  the  west  side  of  the  sun. 
11  is  the  south  edge  of  the  north  wing  on  the  west  side  of  the  sun. 

III  is  the  north  edge  of  the  south  wing  on  the  west  side  of  the  sun. 

IV  is  the  south  edge  of  the  south  wing  on  the  west  side  of  the  sun. 
V  is  the  south  edge  of  the  south  wing  on  the  east  side  of  the  sun. 

VI  is  the  north  edge  of  the  south  wing  on  the  east  side  of  the  sun. 

VII  is  the  south  edge  of  the  north  wing  on  the  east  side  of  the  sun. 

VIII  is  the  north  edge  of  the  north  wing  on  the  east  side  of  the  sun. 

I  have  measured  on  the  negatives  the  distance  from  the  Moon's 
centre  to  the  point  where  each  of  these  faint  edges  terminates. 
The  measures  are  entirely  independent  and  have  been  frequently 
repeated.  It  will  be  seen  from  the  table  below  that  the  further 
one  goes  from  the  Moon's  centre  the  wider  apart  are  the  edges 
VIII  and  V. 


Solar  Eclipse  of  December,  1889. 


TABLE  I.—  U.  S.  X.  O.  CAMERA  NEGATIVES. 


38  & 


11 


IS! 

*3~ 
fl& 


gig 

»  =  s 

£!? 


E.5IB' 

i— i  ®  "  3 
— 'P   r*~l 

&1? 


S=5 

CP  re  re 


1* 

2* 
3 
5 

7t 

Sec. 
5 
10 
15 
20 
23+ 

82 
71 

82+ 
77+ 
53 

86 
71 
85 
85 
57 

46 
40 
46 
41 

77 
66 
72 
82 
63 

72 

70 
71 

77 
62 

SIX-INCH  CLARK  TELESCOPE  NEGATIVES. 


It 

2 

2 
5 

Telescope 
68 

jarred. 
67 

42 

55 

60 

3 

/ 

70 

77 

39 

60 

58 

4J 

10 

56 

67 

35 

52 

60 

5 

25 

60 

70 

42 

65 

62 

Last§ 

(?) 

2-3 

2-3 

2-3 

2-3 

NEGATIVE  OF  THE  TOTAL  PHASE. 

By  Monsieur  L'HOTE. 

Monsieur  HENRI  L'HOTE,  agent  comptable  de  1'hopital  mili- 
taire  of  Cayenne,  was  kind  enough  to  present  to  the  expedition 
a  negative  of  the  total  phase,  taken  by  himself. 

The  focus  of  his  camera  was  17  cm,  the  aperture  of  the 
lens  was  3  cm,  and  a  stop  of  1  cm  was  employed.  The  ex- 
posure was  fifteen  seconds  on  a  MONCKHOVEN  dry  plate. 

There  are  no  evidences  of  clouds  in  the  sky,  though  the  ex- 
posure is  probably  too  long  to  have  shown  them.  The  corona 
extends  out  to  20'  from  the  Moon's  limb.  It  is  much  over- 
exposed. 


PHOTOGRAPHIC  PHOTOMETRY  OF  THE  CORONA. 

The  first  satisfactory  photographs  of  the  corona  were  made 
by  DE  LA  RUE  in  1860.     Since  that  time  nearly  every  eclipse 

*  Negatives  1  and  2  were  standardized. 

t  The  Sun  came  out  on  7  after  III  contact. 

t  Plates  1  and  4  were  standardized. 

§  Plate  " Last"  was  spoiled  by  the  Sun  coming  out  on  it. 


Introduction  by  Mr.  H olden. 


has  been  photographed  more  or  less  successfully.  The  object 
of  such  photographs  was  to  obtain  pictorial  representations  of 
the  corona,  which  should  show  its  forms  and  details  and 
gradations  of  light,  and  which  should  replace  the  hurried  and 
inaccurate  sketches  of  artists  and  others  by  unimpeachable, 
exact,  and  automatic  records. 

It  is  evident  that  the  benefit  which  photography  has  bestowed 
in  this  respect  alone  is  of  the  highest  value. 

But*  photographs  of  the  corona  are  capable  of  more  uses  than 
the  very  important  one  of  giving  forms,  outlines,  etc.  They 
register  the  gradations  of  the  coronal  light  and  are  eminently 
suitable  for  exact  photometric  measures. 

There  are  two  main  problems  which  can  be  solved  by  their 
means,  and  both  are  of  great  importance.  The  first  is  to  de- 
termine the  law  according  to  which  the  coronal  light  is  distrib- 
uted at  each  particular  eclipse,  with  the  ultimate  object  of 
comparing  the  results  obtained  from  different  eclipses  among 
themselves.  The  second  is  to  measure  the  total  light  of  the 
corona  at  each  eclipse  in  order  that  a  comparison  may  be  made 
between  the  results  from  different  eclipses.  We  know  that  the 
corona  varies  enormously  in  form  and  in  brilliancy  at  different 
times.  The  laws  of  such  variations  must  be  sought  for  in  this 
way.  In  order  to  obtain  the  numerical  data  which  are  required, 
it  is  necessary  to  have  on  each  eclipse  plate  some  standard  unit 
of  light  with  which  the  light  of  various  portions  of  the  corona 
can  be  compared. 

It  was  first  proposed  by  Captain  ABNEY,  R.  E.,  F.  R.  S.,  to  put 
on  the  edge  of  each  plate  a  series  of  standard  squares  produced 
by  a  constant  light  shining  for  known  times  at  a  known  dis- 
tance. These  squares  were  to  be  impressed  by  the  light  and 
then  covered  by  a  piece  of  black  paper.  The  plate  was  then  to 
be  exposed  at  the  eclipse.  When  the  plate  was  developed  the 
corona  and  the  squares  would  appear  on  the  negative.  The 
different  parts  of  the  corona  were  then  to  be  compared  with 
squares  of  various  intensities  (due  to  their  different  exposures), 
and  thus  a  numerical  measure  of  the  light  of  various  parts  of 
the  corona  was  to  be  obtained  in  terms  of  units  given  by  a 
known  terrestrial  light  assumed  constant.  The  total  light  of 
each  corona  could  be  derived  by  summing  up  the  measures  of 
the  light  of  its  various  parts;  and  thus  it  was  at  least  theoret- 


Solar  Eclipse  of  December,  1889. 


ically  possible  to  compare  various  coronas  among  themselves 
in  this  respect. 

So  far  as  I  know,  this  experiment  was  first  tried  by  Mr.  W.  H. 
PICKERING  at  the  eclipse  of  1886.  The  Harvard  College  Observ- 
atory adopted  a  standard  lamp  of  the  CARCEL  pattern,  burning 
pure  Colza-oil.  The  light  of  this  lamp,  shining  through  an 
aperture  of  1  mm  in  radius  for  one  second  upon  a  sensitive 
plate  1  metre  distant,  was  taken  as  one  unit  of  light.  In  prac- 
tice the  light  was  allowed  to  shine  only  upon  small  square 
areas  of  the  plate,  about  three  eighths  of  an  inch  on  a  side. 

The  exposures  usually  given  were  1s,  2s,  4s,  8s,  16s,  32s,  64s, 
etc.  This  standard  had  been  employed  for  some  time  at  the 
Harvard  College  Observatory,  and  is  now  in  use  there  for  many 
photometric  purposes. 

It  is  evident  that  at  least  three  things  are  required  of  a  per- 
fect standard  light,  to  be  compared  photographically  with  a 
given  object.  First,  it  must  give  light  of  a  constant  intensity 
during  the  half  hour  or  so  that  is  required  to  "  standardize  "  a 
set  of  plates;  second,  it  must  give  light  of  the  same  absolute 
intensity  on  different  days  and  in  different  years;  third,  it 
should  have  a  spectrum  in  which  the  light-energy  is  distrib- 
uted according  to  the  same  law  as  the  light-energy  in  the 
particular  object  (as  the  corona)  to  be  photographed. 

This  last  requirement  cannot  be  fulfilled  by  any  known  flame, 
and  it  must  be  given  up,  at  least  for  the  present.  A  source  of 
error  is  thus  inevitably  introduced,  which  is  analogous  to  that 
which  I  have  spoken  of  in  the  Bulletin  du  Comite  Internation- 
ale Permanent  pour  Vexecution  photographique  de  la  Carte  du 
del,  page  297,  paragraph  2,  and  which  depends  not  only  on 
the  difference  of  intrinsic  brilliancy  of  the  lamp  and  of  the 
corona  there  referred  to,  but  which  is  further  complicated  by 
their  difference  in  spectrum. 

If  the  first  requirement  named  above  is  fulfilled,  the  compar- 
ison of  the  squares  and  of  the  coronal  pictures  on  the  different 
plates  at  the  same  eclipse  will  give  results  of  value;  provided 
that  the  plates  are  all  of  the  same  formula,  and  that  the  law 
connecting  the  length  of  exposure  with  the  resulting  darkening 
of  the  film  is  known.  It  is  necessary  that  the  plates  shall  all 
be  made  on  one  formula,  so  that  their  sensitiveness  to  rays  of 
each  particular  wave  length  shall  be  constant.  It  is  also  nee- 


Introduction  by  Mr.  H olden. 


essary  to  know  the  law  connecting  the  length  of  exposure  with 
the  resulting  darkening  of  the  film.  It  is  clear  that  such  a 
law  can  be  determined.  Experiments  by  Captain  ABNEY  led 
him  to  the  result  that  the  darkening  was  proportional  to  the 
time  of  exposure,  and  that  law  was  assumed  as  a  basis  for 
the  reductions  of  the  photometric  measures  in  Mr.  PICKERING'S 
Report  of  1886. 

If  the  second  requirement  above  mentioned  is  fulfilled,  that 
is,  if  the  lamp  gives  out  light  of  a  constant  intensity  from  day 
to  day  and  from  year  to  year,  then  it  is  possible  to  compare  the 
photometric  measures  on  different  eclipses;  provided  that  plates 
of  the  same  formula  are  always  used.  It  is  for  this  reason  that 
at  the  Lick  Observatory  the  plates,  SEED  26,  have  been  used  at 
both  the  eclipses  of  1889,  though  I  have  little  doubt  that  better 
pictorial  results  could  be  obtained  with  slower  plates. 

Such,  I  conceive,  are  the  general  principles  according  to  which 
we  must  strive  for  any  numerical  measures  of  the  brightness 
of  celestial  objects  which  can  be  photographed,  as  the  Moon 
and  planets,  the  nebulae,  comets,  and  the  corona.  And  it 
appears  to  be  of  importance  to  endeavor  to  obtain  such 
measures. 

These  principles,  though  quite  simple,  were  not  thoroughly 
understood  here  when  the  preparations  were  made  to  observe 
the  total  solar  eclipse  of  January,  1889.  The  preparations 
themselves  had  to  be  made  in  some  haste,  and  there  was  no 
time  for  experimenting.  Under  these  circumstances  I  applied 
to  Professor  E.  C.  PICKERING  to  obtain  for  the  Lick  Observatory 
an  exact  copy  of  the  standard  lamp  then  in  use  at  the  Harvard 
College  Observatory,  and  he  was  kind  enough  to  provide  us 
with  a  duplicate  of  his  apparatus,  and  with  a  supply  of  oil 
precisely  the  same  as  that  used  in  his  own  work.  The  lamp  of 
the  Lick  Observatory  was  also  tested  at  the  Harvard  College 
Observatory,  and  was  found  to  give  the  same  results  as  their 
standard  lamp  when  used  beside  it.  We  have  lately  received 
(October,  1890),  again  by  Professor  PICKERING'S  kindness,  a 
standard  plate  made  at  the  Harvard  College  Observatory,  con- 
taining squares  of  1s,  2s,  4s,  8s,  16s,  32s,  64s.  This  plate  was  sent 
to  us  undeveloped,  and  before  developing  it  was  exposed  by  Mr. 
BARNARD  to  the  light  of  our  own  lamp  in  a  similar  manner. 
This  plate  will  be  studied  by  Mr.  LEUSCHNER,  in  connection 


8  Solar  Eclipse  of  December,  1889. 


with  other  test  plates  relating  to  our  own  lamp,  and  the  results 
will  be  published  later. 

OBSERVATIONS  OF  THE  ECLIPSE  OF  JANUARY  1,  1889. 

The  photometric  observations  of  the  January  eclipse  were 
made  according  to  the  methods  just  described,  and  they  are 
given  in  the  report  of  that  eclipse,  p.  11  et  seq.  They  were 
reduced  on  the  principle  laid  down  by  Captain  ABNEY,  namely, 
that  the  time  of  exposure  is  directly  proportional  to  the  conse- 
quent darkening  of  the  film.* 

While  that  report  was  in  preparation,  Mr.  BURNHAM  had 
pointed  out  that  this  law  could  only  be  true  within  limits,  and  he 
had  made  some  experiments  which  seemed  to  be  conclusive  in 
the  matter.  It  was  therefore  determined  before  the  publication 
to  make  a  series  of  experiments  on  the  law  in  question,  and  also 
to  test  the  standard  lamp  to  see,  first,  if  it  remained  constant 
during  thirty  minutes  or  so,  and  second,  whether  it  gave  the 
same  absolute  light  from  day  to  day. 

This  work  had  been  assigned  to  Mr.  LEUSCHNER,  one  of  the 
members  of  the  eclipse  party,  when,  most  unfortunately,  the 
only  chimney  furnished  with  the  standard  lamp  was  broken. f 

A  series  of  annoying  and  unavoidable  delays  made  it  impossi- 
ble to  replace  this  chimney  for  several  months,  and  it  was  finally 
determined  to  print  the  report  as  it  then  stood  with  the  neces- 
sary reserves,  which  was  accordingly  done. 

The  photometric  and  photographic  questions  involved  had 
to  be  put  to  one  side  until  they  could  be  studied  by  Mr.  LEUSCH- 
NER in  his  thesis  for  the  degree  of  Doctor  of  Philosophy.  In 
the  meantime,  Mr.  BURNHAM  and  Mr.  SCHAEBERLE  have  made 
the  experiments  described  in  their  report  (q.  v.),  and  Mr. 
LEUSCHNER  has  obtained  all  the  plates  necessary  for  a  solution 
of  this  question.  He  has,  however,  only  been  able  to  com- 
pletely reduce  and  print  the  results  which  are  given  in  his 
paper  in  the  Publications  of  the  Astronomical  Society  of  the 
Pacific,  Vol.  II,  p.  7.  (Determination  of  the  relation  between 
the  exposure  time  and  the  consequent  blackening  of  a  photo- 
graphic film.)  Mr.  LEUSCHNER'S  results  (which  are  only  prelim- 

*  Report,  p.  13. 

t  Report,  pp.  22,  103. 


Introduction  by  Mr.  H olden.  9 

inary)  were  that  between  exposures  of  2s  and  8s  the  blackening 
of  the  film  was  proportional  to  the  time,  and  that  it  is  likely 
that  the  law  changes  beyond  8s  exposure.  This  applies  to  SEED 
26  plates. 

OBSERVATIONS  OF  THE  ECLIPSE  OF  DECEMBER,  1889. 

The  plates  of  this  eclipse  were  returned  to  the  Observatory 
in  March,  1890,  and  they  were  at  once  measured  and  reduced 
precisely  as  in  the  case  of  those  taken  in  the  preceding  Jan- 
uary. It  is  tolerably  certain  already  that  the  results  from  both 
eclipses  must  be  again  reduced  according  to  different  principles. 
What  the  true  relation  between  the  time  and  the  opacity  of 
the  film  really  is,  cannot  be  stated  at  present,  but  it  is  proba- 
bly not  very  difficult  to  obtain  such  a  law  which  will  be  amply 
accurate  for  all  practical  uses. 

Mr.  LEUSCHNER  has  made  some  preliminary  measures  on  his 
plates  which  bear  on  the  question  of  the  constancy  of  the  light 
from  the  standard  lamp. 

His  results,  briefly  stated,  are  that  the  standard  lamp 
remains  constant  for  an  hour  or  more  (so  that  plates  standard- 
ized on  the  same  day  are  comparable),  but  that  enormous  vari- 
ations occur  between  the  results  of  different  days  (so  that  no 
results  can  be  drawn  from  a  comparison  of  plates  standardized 
at  different  times). 

A  considerable  time  must  elapse  before  the  numerical  results 
of  his  comparisons  can  be  given;  and  therefore  I  have  preferred 
not  to  delay  the  present  report  on  this  account,  but  to  treat  the 
subject  precisely  as  in  the  Eclipse  Report  of  January,  1889. 
The  results  for  each  eclipse,  taken  separately,  will  have  a  cer- 
tain value,  and  the  chief  error  to  which  they  are  subject  will 
be  due  to  the  error  of  the  relation  between  opacity  of  the  film 
and  exposure  time  assumed  on  the  authority  of  Captain  ABNEY. 
The  results  from  the  two  eclipses  cannot  properly  be  compared. 
The  whole  matter  must  be  examined  again  after  the  photo- 
metric experiments  of  Mr.  LEUSCHNER  have  been  discussed. 

PHOTOMETRIC    MEASUREMENTS    OF    THE     DECEMBER     ECLIPSE- 
PLATES. 

The  standardized  plates  were  Nos.  1  and  4  of  the  6-inch 
telescope  and  Nos.  1  and  2  of  the  U.  S.  N.  O.  camera.  Only 


10  Solar  Eclipse  of  December,  1889. 

the  last  three  are  suitable  for  measurement.  On  plate  4  of  the 
telescope  the  measures  are  very  difficult,  but  the  results  by  Mr. 
BARNARD  and  myself  are: 

Brighest  part  of  the  corona  matches  square  80  seconds. 
Polar  rays  (average)  match  square  45  seconds. 
Sky  (average)  matches  square  2£  seconds. 

Hence,  paying  no  regard  to  the  absorption  of  the  lens  as  yet, 

we  have: 

Brightest  part  of  the  corona     =  0.0209    units. 
Polar  rays  (average)  —  0.0117    units. 

Brightness  of  the  sky  (average)  =  0.00065  units. 

The  units  here  employed  are  intended  to  be  the  same  as  those 
of  the  Harvard  College  Observatory,  and  the  same  as  those  for 
the  January  eclipse.  The  absorption  coefficient  of  this  lens  is 
1.39.  Hence  the  results  above  become: 

Brightest  part  of  the  corona     =  0.029      units. 
Polar  rays  (average)  =  0.016      units. 

Brightness  of  the  sky  —  0.00090  units. 

The  polar  rays  are  eighteen  times  as  bright  as  their  back- 
ground. 

The  measures  on  the  camera  plate  No.  1  are: 

Sky  (average)  matches  the  square  exposed  20  seconds,  or  its 
brightness  (without  regard  to  absorption)  is  0.00074  units. 

The  brightest  parts  of  the  corona  are  brighter  than  the 
square  with  the  longest  exposure,  and  therefore  cannot  be 
directly  measured. 

The  measures  on  the  camera  plate  No.  2  are  difficult.  The 
sky  within  2^  degrees  from  the  Sun  matches  square  70  on  the 
average.  In  some  places  the  sky  is  as  faint  as  50,  in  some  as 
bright  as  90;  70  is  probably  the  fairest  average,  though  the 
result  is  not  satisfactory.  This  measure  makes  the  brightness 
of  the  sky  0.001 29  units. 

The  absorption  coefficient  of  this  lens  is  1.14. 

Hence  the  camera  plates  Nos.  1  and  2  give: 

Brightness  of  the  sky,  No.  1  =  0.00084. 
No.  2  -=  0.00147. 

The  first  of  these  measures  is  to  be  preferred.  In  most  of 
these  measures  I  have  had  the  benefit  of  Mr.  BARNARD'S  advice. 


Introduction  by  Mr.  H olden.  n 


TOTAL  LIGHT  OF  THE  CORONA. 

Mr.  BARNARD  has  measured  the  telescope  plate  No.  4  by  the 
method  which  he  has  described  in  the  Report  of  the  Eclipse  of 
January  1,  1889  (page  62),  and  has  derived  the  contour  lines 
which  are  given  in  Plate  IX.  This  diagram  has  been  trans- 
ferred to  a  piece  of  pasteboard  and  weighed  precisely  as  described 
on  page  12  of  the  report  above  mentioned. 

The  results  are: 

Area  of  the  Sun  =  833.6  square  minutes  =  weighs  2.08  grammes. 
Area  d — Sun  =  452.8  square  minutes  =  weighs  1.13  grammes. 
Area  c—d  =  140.3  square  minutes  =  weighs  0.35  grammes. 

Area  6 — c  =  184.3  square  minutes  =  weighs  0.46  grammes. 

Area  a — b  — -  689.2  square  minutes  =  weighs  1.72  grammes. 

Area  k— a  =  913.5  square  minutes  =  weighs  2.28  grammes. 

The  curve  d  matches  square  70. 
The  curve  c  matches  square  60. 
The  curve  6  matches  square  40. 
The  curve  a  matches  square  20. 
The  curve  k  matches  square  10. 

I  have  assumed  the  area  between  k  and  a  to  match  square 
10;  the  area  between  a  and  b  to  match  square  20;  the  area 
between  6  and  c  to  match  square  50;  the  area  between  c  and 
d  to  match  square  60;  and  the  area  between  d  and  the  Sun  to 
match  square  70.  Or,  in  other  terms,  the  intrinsic  brilliancies 
are  0.00261,  0.00522,  0.01305,  0.01566,  0.01827,  respectively 
(always  without  taking  the  absorption  of  the  lens  into  account). 

Assuming  the  square  minute  of  arc  as  the  unit-area,  the 
total  brightness  of  the  corona  becomes  18.85  units;  or,  correct- 
ing for  absorption  by  multiplying  by  1.39,  the  total  actinic 
brightness  of  the  corona  is  26.20  units. 


THE  STANDARDIZED  PLATES. 

Some  of  the  eclipse  plates  received  the  standard-squares  for 
exposures  of  5,  10,  15,  20,  30,  40,  50,  60,  70,  80  seconds,  pre- 
cisely as  described  in  the  report  of  the  January  eclipse.  The 
results  from  these  plates  have  just  been  given.  Besides  the 
plates  to  be  exposed  at  the  eclipse,  Mr.  BARNARD  standardized 
ten  others— A,  B,  C,"D,  E,  F,  G,  H,  I,  J  (SEED  26)— on  Septem- 
ber 24,  1889. 


12          »       Solar  Eclipse  of  December,  1889. 

A,  B,  C,  D  were  taken  with  others  to  the  eclipse,  and  then 
returned  to  the  Lick  Observatory.  A  and  B  were  developed 
on  the  day  after  the  eclipse  by  Mr.  BURNHAM.  (They  arrived 
at  the  Lick  Observatory  on  March  5,  1890.)  C  and  D  were 
brought  back  to  the  Observatory,  and  developed  here  by  Mr. 
BARNARD  on  their  return  (March  17,  1890).  E,  F,  G,  H  re- 
mained at  the  Observatory.  E  and  F  were  developed  by  Mr. 
BARNARD  on  December  22,  1889.  G  and  H  were  developed  at 
the  same  time  with  C  and  D.  I  and  J  were  developed  by  Mr. 
BARNARD  immediately  after  they  were  exposed,  on  September 
24,  1889.* 

TEST  PLATES  —  FIRST   SERIES  OF   STANDARD    SQUARES    (Put  on 
September  24,  1889). 

The  chronological  order  of  the  development  of  the  test  plates 
for  the  squares  of  Series  I  (September  24)  was  then  I  and  J 
(L.  0.,  September  24);  E  and  F  (L.  O.,  December  21);  A  and 
B  (Cayenne,  December  22);  C,  D,  G,  H  (L.  O.,  March  17). 
Mr.  BARNARD'S  measures  give,  when  transformed  (see  his  report 
following): 

(A'=0.94J'  ,.,x   <E'=1.28J'  ,~  T,     T, 

•>  }B'=0.93J'  ('3MF'=1.01J'  (5)I=J 

j  C'=0.55  J'  m  J  G'=0.38  J' 

'>  |  D'=0.  79  J'  tj  |H'=1.10J' 


These  equations  express  A',  B',  etc.,  all  in  terms  of  the  same 
unit,  viz.:  J'.  But  as  J'  was  not  developed  at  the  same  time  as 
A',  B',  etc.,  it  does  not  follow  that  1.00  A',  etc.,  ought  to  equal 
1.00  J'.  So  far  as  the  evidence  is  sufficient,  the  above  compari- 
sons show  that  all  plates  taken  directly  from  the  box,  standard- 
ized and  exposed  immediately,  would  have  given  similar  results 
(5).  Equations  (3)  show  that  on  December  21,  plates  remaining 
at  the  L.  0.  might  vary,  say  30  per  cent  among  themselves,  if  we 
assume  the  lamp  as  constant  during  the  short  time  required  to 
standardize  the  plates,  which  we  have  reason  to  do.  (4)  shows 
that  by  March  17,  1890,  two  plates  remaining  at  the  L.  O. 
actually  did  vary  72  per  cent  under  the  same  supposition. 
Equations  (1)  show  that  two  Cayenne  plates,  developed  Decem- 

*The  plates  A,  B,  C,  D,  E,  F,  G,  H,  I,  J  also  received  squares  of  exposures 
5.  10.  15,  20,  30,  40,  50,  60,  70,  80  seconds. 


Introduction  by  Mr.  H olden.  13 

her  22,  were  practically  identical  with  the  normal  plates  I  and 
J;  though  it  was  possible,  from  (3),  that  other  such  plates 
might  have  varied  among  themselves  as  much  as  or  more  than 
27  per  cent.  Equations  (2)  would  seem  to  show  that  the 
return  journey  to  the  United  States,  and  the  lapse  of  time 
might  lead  us  to  expect  a  change  of  something  like  24  per  cent 
among  such  plates,  relatively  to  each  other.  It  is  not  practica- 
ble to  say  what  absolute  changes  are  to  be  expected,  owing  to 
the  different  development  above  described. 

If  Mr.  LEUSCHNER'S  subsequent  measures  bear  out  those  which 
he  has  made  up  to  this  time,  that  is,  if  they  prove  that  the  stand- 
ard lamp  gives  light  of  a  constant  intensity  for  a  half  an  hour 
or  more,  then  it  follows  that  a  considerable  part  of  the  changes 
shown  by  the  foregoing  equations  is  due  to  alterations  in  the 
sensitiveness  of  the  films,  and  only  a  relatively  insignificant 
part  to  changes  in  the  lamp.  Such  changes  in  the  sensitive- 
ness of  the  films  would  hardly  be  detected  in  the  taking  of 
ordinary  landscapes,  where  the  longer  or  shorter  development 
of  the  plate  comes  in  to  correct  all  errors  of  exposure-time,  or 
of  varying  sensitiveness. 

TEST  PLATES — SECOND  SERIES  OF  STANDARD  SQUARES  (Put  on 
March  16,  1890). 

A  second  series  of  squares  was  put  on  plates  C,  D  (Cayenne), 
G,  and  H  (Lick  Observatory),  by  Mr.  BARNARD  on  March  six- 
teenth, and  these  plates  were  developed  together  on  March 
seventeenth. 

Mr.  BARNARD'S  measures  give,  by  a  comparison  between  the 
squares  of  the  second  series  only: 

(C"=0.61H" 

(6)  ^"==0.67  H" 
(G"=0.36  H" 

.    From  the  first  series  only  we  have: 

(C'=0.63  H' 

(7)  -m'=0.55H' 
(G'=1.35  H' 

If  we  take  H  as  the  standard,  it  would  seem  that  no  great 
change  took  place  in  C  and  D  between  the  times  when  the  first 
and  second  series  of  squares  was  put  on,  or  that  C,  D,  and  H 
varied  together,  according  to  the  same  law.  If,  however,  we 


14 


Solar  Eclipse  of  December,  1889. 


employ  G  as  the  standard,  or  the  mean  between  G  and  H,  there 
will  have  been  an  enormous  change.  If  we  express  the  inten- 
sity of  the  second  series  of  squares  in  terms  of  brightness  of  J 
(which  has  squares  of  the  first  series  only),  we  have: 

(C"=0.27J';  C"+D" 

|D"=0.37J';      2 

[G"=0.61J';  G'4-H' 

'H"=0.45J';     2 


(8) 


(9) 


).53  J' 


We  do  not  yet  know  what  variations  we  may  expect  in  the 
absolute  intensity  of  the  standard  lamp  flame,  but  wre  do  know 
that  these  are  very  great. 

In  the  absence  of  any  numerical  data,  I  am  inclined  to  attrib- 
ute by  far  the  largest  part  of  the  variations  shown  by  equations 
(6),  (8),  and  (9)  to  actual  differences  in  the  absolute  intensity 
of  the  lamp  flame  on  the  two  dates  upon  which  the  two  sets  of 
squares  were  impressed  (September  24,  1889,  and  March  16, 
1 890) .  We  can,  then,  draw  no  conclusions  from  these  equations. 
Under  the  assumptions  previously  made,  we  can  bring  the 
results  from  the  three  eclipses  of  1886,  January,  1889,  and 
December,  1889,  into  the  following  table: 

TABLE  II.— PHOTOMETRIC  RESULTS. 


PICKERING— 
August,  1886. 

HOLDEN— 
January,  1889. 

HOLDEN— 
December,  1889. 

Intrinsic  actinic  brilliancy  of  the 
brightest  parts  of  the  corona  
Intrinsic  actinic  brilliancy  of  the 
polar  ravs  (about)  

0.031 

0.079 
0.053 

0.029 
0016 

Intrinsic  actinic  brilliancy  of  the 
skv  near  corona  . 

0.0007 

00050 

00009 

Total  actinic  light  of  the  corona  ... 
Total  actinic  light  of  the  sky 

37. 

52000. 

60.8 
185625 

26.2 
33412 

Ratio  of  total  coronal  to  total  sky 
light  (actinic) 

1  to  1  400 

1  to  3  043 

1  to  1  985 

Ratio  of  intrinsic  brilliancy  of  the 
brightest  parts  of  the  corona  to 
that  of  the  sky  (actinic)...  

44  to  1 

16  to  1 

32  to  1 

Intrinsic  actinic  brilliancy  of  the 
sky  at  1°  from  the  Sun  in'daylight 
(average)  

40. 

Intrinsic  actinic  brilliancy  of  the 
full  Moon  ,_.. 

1.66 

Total  actinic  light  of  the  full  Moon 
(SD=16'.75)  

1,461.5 

Intrinsic  actinic  brilliancy  of  sky 
within  5°  of  the  full  Moo"n 

0.000064 

Magnitude  of  the  faintest  star 
shown  on  the  eclipse  photographs  . 

2.3 

Introduction  by  Mr.  H olden.  15 

The  differences  between  the  results  of  January  and  of  Decem- 
ber, 1889,  are  very  striking,  when  we  regard  the  measures  as 
absolute.  If,  however,  we  take  the  relative  brightness  of  the 
various  features  at  both  eclipses,  there  is  greater  harmony.  A 
priori,  the  results  of  January  are  to  be  preferred,  as  the  atmos- 
pheric conditions  were  far  more  favorable  at  this  eclipse. 

None  of  the  results  is  to  be  considered  as  final,  as  it  is  prob- 
able that  all  the  reductions  must  be  made  anew,  for  reasons 
already  given. 

A  few  words  may  be  said  in  comparison  of  the  instruments 
and  programmes  of  the  two  eclipses  of  1889,  in  order  to  bring 
out  the  information  gained  by  the  experience  at  the  two  eclipses. 

The  definition  of  the  central  parts  of  the  6-inch  CLARK  object- 
ive is  certainly  not  inferior  to  the  definition  of  the  telescope 
employed  in  January,  as  is  shown  by  capital  photographs  of 
the  Moon  and  of  stars,  which  Mr.  BARNARD  has  made  by  its  use. 
The  ratio  of  aperture  to  focus  was  almost  exactly  the  same  for 
both  instruments.  The  Sun  was  substantially  at  the  same  alti- 
tude at  both  stations.  The  same  plates  were  used  (SEED  26) 
on  both  expeditions,  and  the  same  care  in  development.  It  is 
quite  possible  that  the  December  plates  were  slightly  more  sen- 
sitive than  those  used  in  January,  as  the  former  were  specially 
ordered  from  the  SEED  Company,  while  the  latter  were  bought 
in  the  market. 

Mr.  BARNARD'S  negatives  of  January,  1889,  were  exposed  for 
one,  three,  and  four  and  one  half  seconds,  and  it  is  certain  that 
the  latter  is  the  best  negative  in  every  respect,  both  as  to  detail 
and  as  to  extent.  It  is  also  almost  certain  that  an  exposure  of 
five,  six,  or  seven  seconds  at  the  January  eclipse  would  have 
produced  still  finer  results.  With  these  facts  in  mind,  the 
shortest  exposure  with  the  6-inch  telescope  for  the  eclipse  of 
December  was  fixed  at  two  seconds.  An  examination  of  Mr. 
BURNHAM'S  Negative  1  (exposed  two  seconds)  shows  that  it  is 
very  much  over-exposed,  and  that  an  exposure  time  of  one  sec- 
ond, or  even  less,  would  have  been  much  nearer  the  mark  at  that 
time. 

I  believe  if  the  air  had  been  clear  and  dry  at  Cayenne,  as  it 
was  in  January,  at  Bartlett  Springs,  that  the  exposures  given 
would  have  been  found  to  be  the  right  ones. 


16  Solar  Eclipse  of  December,  1889. 

As  it  was,  the  programme  should  certainly  have  included  at 
least  one  short  exposure,  in  order  to  cover  the  very  case  that 
arose.  The  same  remarks  apply  to  the  negatives  with  the 
DALLMEYER  camera,  with  the  additional  provision  that  the 
aperture  should  have  been  about  four  inches. 

It  is  to  be  remembered  that  the  detail  of  the  inner  corona 
can  hardly  be  satisfactorily  given  in  a  camera  of  less  than  50 
inches  focus.  It  then  appears  to  be  best  to  use  cameras  of  30 
inches  focus  or  less,  in  obtaining  negatives  principally  designed 
to  show  the  outer  parts  of  the  solar  corona,  and  to  sacrifice  the 
inner  coronal  details,  as  was  intentionally  done  in  the  Decem- 
ber eclipse  pictures  taken  with  the  DALLMEYER  camera. 

If  the  same  eclipse  were  to  be  observed  again,  under  unknown 
circumstances  as  to  weather,  it  is  my  opinion  that  the  pro- 
gramme actually  followed,  with  the  additions  which  I  have  just 
indicated,  would  be  the  proper  one  to  follow. 

In  the  report  following,  the  writers  advocate  the  photograph- 
ing of  future  eclipses  by  expert  photographers  entirely  unem- 
barrassed by  any  instructions  as  to  the  times  of  exposure.  They 
would  have  the  observer  spend  a  certain  small  part  of  the 
totality  in  examining  the  corona  with  the  eye,  and  in  choosing 
a  suitable  set  of  exposures  at  the  instant.  With  this  view  I 
cannot  agree,  and  it  appears  to  me  that  Mr.  BURNHAM'S  experi- 
ence at  the  December  eclipse  is  a  complete  refutation  of  this 
proposal.  As  Mr.  BURNHAM  had  expressed  the  same  view  before 
going  to  Cayenne,  the  programme  of  work  for  his  telescope  was 
purposely  left  incomplete  in  order  to  allow  him  this  very  lib- 
erty. Considerably  more  than  20  seconds  was  available  to  him 
after  the  prescribed  exposures  were  made  with  the  telescope. 
There  is  now  no  doubt  that  an  exposure  of  about  one  second 
was  the  correct  one  for  this  instrument.  The  exposure  actually 
made  was  certainly  twenty  times  as  much,  and  the  Sun  reap- 
peared while  the  plate  was  yet  exposed.  If  this  could  occur 
in  such  a  case,  it  is  far  more  likely  to  happen  to  an  observer  of 
less  experience,  and  especially  if  an  eclipse  is  viewed  for  the 
first  time. 

It  appears  to  me  to  be  the  sound  principle  to  lay  down  a 
programme  based  on  previous  experience,  and  to  follow  this 
exactly. 

The  range  of  exposures  must  be  great  enough  to  cover  all 


Introduction  by  Mr.  H olden.  17 

ordinary  weather  conditions.  The  mistake  in  the  present  case 
was,  I  think,  in  not  definitely  prescribing  at  least  one  very 
quick  exposure  for  the  CLARK  telescope,  and  a  reduction  of  the 
aperture  to  four  inches  for  the  DALLMEYER  camera. 

EXTENSION  OF  THE  OUTER  CORONA. 

The  negatives  of  the  December  eclipse  do  not,  of  themselves, 
lead  to  the  suspicion  of  the  existence  of  this  feature.  The  exact 
evidence  which  they  yield  is  presented  in  Table  I. 

On  the  other  hand,  when  these  negatives  are  examined  with 
the  special  object  of  finding  such  a  feature,  they  yield  no  evi- 
dence against  it.  In  fact  they  show  that  the  outer  corona  is 
some  45'  wide  at  80'  from  the  Moon's  centre,  and  that  the  begin- 
ning of  the  trumpet-shaped  form  is  present.  While  it  is  to  be 
regretted  that  the  December  negatives  are  not  decisive  on  this 
point,  this  fact  has  little  or  nothing  to  do  with  the  evidence 
upon  which  the  existence  of  the  extension  of  the  outer  corona 
rests. 

I  may  be  permitted  to  recapitulate  this  evidence  as  follows: 
All  of  Mr.  BARNARD'S  negatives  of  January,  1889,  show  a 
strongly  marked  divergence  in  the  edges  of  the  outer  corona 
beyond  the  55'  circle,  and  his  negative  "  C  "  enables  us  to  trace 
this  trumpet-shaped  extension  to  75'  or  so.  The  negatives  of 
Messrs.  LOWDEN  and  IRELAND  show  the  same  outlines  to  130' 
and  more. 

The  negatives  of  Father  CHARROPPIN  show  the  same  thing  in 
a  beautiful  manner  out  as  far  as  100'  or  more.  The  same  ex- 
tension is  more  or  less  plainly  shown  on  the  negatives  of  Messrs. 
DORNIN,  JOHNSON,  TREAT,  PASSAVANT,  GRIMWOOD,  LANGE,  BURCK- 
HALTER,  and  TABER.  These  negatives  were  made  by  eleven 
different  instruments  at  four  widely  separated  observing  stations. 
Moreover,  the  naked-eye  drawing  of  Miss  TREAT  shows  the  same 
feature  exactly.  It  therefore  appears  to  be  certain  that  the 
extension  of  the  outer  corona  first  photographed  in  January, 
1889,  has  an  objective  existence.  The  negatives  of  December, 
1889,  are  not  sufficient  to  prove  the  existence  of  such  a  feature; 
but,  so  far  as  they  give  any  evidence  at  all,  they  confirm  that 
obtained  in  the  previous  January. 

The  Eclipse  Committee  of  the  Royal  Astronomical  Society 
2 


18  Solar  Eclipse  of  December,  1889. 


considered  it  "doubtful  whether  this  extension  has  been  pho- 
tographed," and  made  a  programme  for  the  December  eclipse 
which  was  designed  to  decide  the  question.  It  appears  to  have 
been  the  idea  of  the  committee  that  with  two  instruments  of 
different  light  ratios,  "//,  the  extension  would  necessarily  be 
greater  (for  the  same  exposure)  in  that  instrument  having  the 
greater  light  ratio.  In  their  Report  (Mon.  Not.,  R.  A.  S.,  Vol. 
50,  p.  4)  it  is  said:  "The  failure  of  exposures  of  say  three  min- 
utes to  give  a  sensibly  greater  extension  than  one  minute  is 
adduced  by  Captain  ABNEY  as  a  reason  for  believing  the  evi- 
dence to  be,  on  the  whole,  against  the  reality  of  coronal 
streamers."  Special  mirrors  were  constructed,  of  aperture  15 
inches,  focus  45  inches,  for  use  at  the  December  eclipse;  "the 
chief  point  in  the  use  of  the  mirrors  is  to  get  long-exposure 
pictures.  Short  exposures  will  also  be  of  interest,  but  the 
question  the  mirrors  were  built  to  settle  is  the  reality  of  the 
coronal  extension"  (by  employing  long  exposures).  In  the 
Monthly  Notices  (Vol.  50,  p.  271)  the  Secretary  of  the  Eclipse 
Committee  has  given  a  preliminary  account  of  the  negatives 
secured  by  the  use  of  the  mirrors  above  described  ("/,—%)  and 
of  cameras  ("//— TT)-  The  plates  taken  with  the  mirror  used 
in  South  America  showed  no  greater  extension  than  those  taken 
with  the  camera. 

The  sky  was  obscured  at  the  African  station,  and  no  com- 
parison can  be  made  between  the  performance  of  the  instru- 
ments used  there. 

"It  cannot  be  said  that  any  definite  conclusion  has  been 
arrived  at  with  regard  to  the  extension.  It  is  almost  certain 
that  for  some  cause  the  20-inch  mirror  was  not  efficient  on  the 
occasion  of  the  eclipse,  and  it  is  probable  that  it  was  dewed. 
With  an  effective  aperture  of  15  inches,  the  short  exposure 
plates  should  have  shown  much  more  if  the  mirror  had  been 
in  its  normal  state.  Hence  the  failure  to  photograph  the 
corona  more  than  about  a  diameter  from  the  limb  in  40  sec- 
onds cannot  be  taken  as  evidence  against  the  possibility  of 
photographing  'the  extension'  in  the  future"  (with  long  ex- 
posures). 

It  appears  to  me  that  the  questions  involved  should  be  re- 
garded somewhat  differently.  If  it  is  desired  to  photograph  a 
faint  nebula  or  star  on  the  background  of  a  perfectly  dark 


Introduction  by  Mr.  H olden.  19 

night-sky,  the  method  above  suggested  is  the  appropriate  one. 
If,  however,  it  is  wished  to  record  the  slight  contrast  between 
the  corona  and  a  sky  which  is  by  no  means  dark,  it  must 
necessarily  fail,  as  can  readily  be  proved  by  attempting  to  pho- 
tograph light,  fleecy  clouds  near  the  Sun  (when  the  latter  is 
temporarily  covered  by  a  cloud)  in  a  daylight  sky.  Even  with 
quite  short  exposures,  the  slight  contrasts  are  lost,  and  longer 
exposures  give  a  uniform  background.  As  an  example,  I  may 
refer  to  experiments  by  Mr.  BURNHAM  (with  a  camera  a=J 
inch,  /— 9,  stop=732>  plate  SEED  26)  on  photographing  fleecy 
clouds  near  the  totally  obscured  Sun  (which  was  about  twenty  - 
five  degrees  above  the  western  horizon).  He  took  four  plates 
with  times  of  one  fourth,  one  eighth,  one  sixteenth,  and  one 
thirty-second  of  a  second.  The  plates  were  from  the  same  box, 
and  were  developed  together.  There  is  very  great  improve- 
ment in  the  faint  contrasts  of  cloud  and  fog  as  the  time  be- 
comes shorter  and  shorter,  and  there  is  no  doubt  that  a  time  of 
one  sixty-fourth  second  or  less  would  have  given  even  better 
results.* 

The  visual  contrast  between  a  faint  nebula  and  a  very  dark 
sky  may  be  the  same  as  the  contrast  between  a  fairly  bright 
corona  and  a  fairly  bright  sky,  and  yet  the  two  objects  must  be 
photographed  according  to  different  methods.  The  dark  sky 
has  little  or  no  effect  on  the  plate,  and  therefore  the  greater  the 
light-ratio  of  the  camera  and  the  longer  the  exposure,  the  more 
of  the  nebula  is  shown.  On  the  other  hand,  the  sky  at  a  total 
eclipse  is  actinically  fairly  bright  (about  one  tenth  as  bright  as 
the  polar  rays  in  January,  1889),  and  if  the  camera  has  a  great 
light-ratio  and  the  exposure  is  prolonged  beyond  a  certain  limit, 
the  slight  contrast  between  the  sky  and  the  fainter  corona  will 
inevitably  be  lost.f 

The  problem  of  photographing  the  outer  corona  is  the  same 

*  These  plates  are  preserved  at  the  Lick  Observatory  for  reference. 

t  M.  A.  de  la  BAUME  PLUVINEL  photographed  the  eclipse  of  December,  from 
a  point  near  Cayenne,  with  five  cameras  of  different  light-ratios  mounted  on 
the  same  stand.  He  says  of  his  results  (Comptes  Rendus,  1890,  February, 
quoted  in  Nature):  "  Une  premiere  comparaison  des  cinq  e"preuves  montre 
que  les  objectifs  les  plus  lumineux  n'ont  pas  donnas  des  images  plus  com- 
pletes que  les  objectifs  les  moins  lumineux.  L'emploi  d'instruments  trop 
puissants  n'est  pas  meme  a  recommander,  car  1 'image  qu'ils  donnent  du  ciel 
peut  etre  assez  intense  pour  se  confondre  avec  1'image  des  regions  peu  lumi- 
neuscs  de  la  couronne." 


20  Solar  Eclipse  of  December,  1889. 

as  that  of  photographing  light  clouds  near  the  Sun,  or  a  star 
in  the  daytime;  and  it  appears  that  the  failure  of  the  mirror 
of  the  British  expedition  to  show  more  extension  than  the 
camera,  could  have  been  predicted  even  for  the  shorter  expos- 
ures, and  still  more  for  the  longer  ones. 

An  excellent  illustration  of  the  two  methods  may  be  had  by 
employing  the  same  instrument:  First,  to  photograph  the  earth- 
light  on  the  Moon  in  the  evening  sky;  and  second,  to  photo- 
graph the  Moon  itself  in  daylight.  In  the  first  case,  the  sky 
has  little  actinic  effect,  and  the  exposure  may  consequently  be 
made  quite  long,  several  minutes,  for  example.  (See  a  note 
on  this  subject  by  Mr.  BARNARD,  in  the  Publications  A.  S.  P., 
No.  8.)  In  the  second  instance,  the  quickest  exposures  will 
alone  give  good  results.  As  an  example,  I  may  quote  negatives 
made  with  the  great  telescope  (*//•=  VtT.s)  on  April  23,  1890, 
with  the  Moon  nearly  on  the  meridian,  about  4  p.  M.  An  ex- 
posure of  YIO  second  on  SEED  26  plates  gave  a  good  contrast 
between  the  limb  of  the  Moon  and  the  sky.  Other  negatives 
taken  April  twenty-sixth,  at  2  p.  M.,  with  the  aperture  con- 
tracted to  fifteen  inches  ("//—-$?)  and  exposure  l/10  second  on 
similar  plates,  are  far  more  satisfactory,  as  the  details  on  the 
Moon's  surface  begin  to  show.  Negatives  taken  of  Alpha  Lyrse 
in  broad  daylight,  with  contracted  apertures,  have  also  a  bear- 
ing on  this  question.  (See  Publications  of  the  Astronomical 
Society  of  the  Pacific,  Vol.  II,  page  250.) 

CONCLUSION. 

On  page  19  of  the  Keport  of  the  Eclipse  of  January  last,  I 
gave  certain  conclusions  which  it  seemed  to  me  could  fairly  be 
drawn  from  the  observations  of  that  eclipse  and  of  preceding 
eclipses.  If  the  mechanical  theory  of  the  corona  advanced  by 
Professor  SCHAEBERLE  in  the  present  volume  be  not  true,  I  see  no 
changes  to  be  made  in  the  conclusions  heretofore  given.  If,  how- 
ever, as  I  believe,  the  theory  of  the  corona  proposed  by  Professor 
SCHAEBERLE  is  a  correct  explanation  of  the  phenomena  of  the 
coronal  forms  observed  at  all  past  eclipses,  and  is  adequate  to 
predict  the  general  forms  of  future  phenomena  of  the  sort,  then 
serious  modifications  are  required  in  the  conclusions  above 
referred  to.  For  example,  the  observed  and  indisputable  fact 


Introduction  by  Mr.  H olden.  21 

that  the  coronas  of  1867, 1878,  and  1889  are  of  the  same  strongly 
marked  type,  must  be  attributed  to  the  situation  of  the  Earth 
with  respect  to  the  plane  of  the  solar  equator,  and  not  to  the 
accidental  circumstance  that  the  years  1867,  1878,  and  1889 
were  all  years  of  minimum  Sun  spots.  As  in  this  case,  so  in 
others.  The  changes  which  are  necessitated  by  the  acceptance 
of  Professor  SCHAEBERLE'S  theory  can  be  easily  made  by  any 
one  who  comprehends  the  theory;  and  I  will  not  dwell  further 
upon  them.  I  think  it  worth  while,  however,  to  call  attention 
to  the  fact  that  the  excellent  observations  of  the  eclipse  of  last 
January,  obtained  by  the  Lick  Observatory  party  and  by  the 
expedition  of  the  Amateur  Photographic  Association  (as  well 
as  by  other  parties  whose  reports  are  not  in  print  at  the  time 
of  writing  this),  furnished  a  sure  basis  for  investigations  of  the 
sort,  when  compared  with  those  made  in  December.  It  is  a 
source  of  legitimate  pride  to  all  connected  with  the  Lick  Observ- 
atory that  nothing  was  neglected  in  its  two  eclipse  expeditions 
of  1889  to  insure  satisfactory  results,  and  it  is  a  matter  of  con- 
gratulation that  the  weather,  which  was  most  favorable  in 
January,  was  not  entirely  unpropitious,  though  still  very 
unfavorable,  at  the  December  eclipse. 

EDWARD  S.  HOLDEN. 
LICK  OBSERVATORY,  October,  1890. 


22  Solar  Eclipse  of  December,  1889. 


II -REPORT  OF  S.  W.  BURNHAM  AND  1.  M.  SCHAEBERLE. 


THE  TOTAL  ECLIPSE  OF  DECEMBER  21-22,  1889. 

The  expedition  from  the  Lick  Observatory  to  observe  the  total 
eclipse  of  December  21-22,  1889,  at  Cayenne,  French  Guiana, 
was  the  result  of  a  generous  donation  for  this  special  object 
from  Colonel  CHARLES  F.  CROCKER,  of  San  Francisco.  Ample 
funds  were  given  to  equip  the  party,  consisting  of  S.  W.  BURN- 
HAM  and  J.  M.  SCHAEBERLE,  in  the  most  complete  and  liberal 
manner,  and  to  provide  for  all  necessary  disbursements  at 
Cayenne,  and  on  the  long  voyages  going  to  and  returning  from 
that  little  known  and  out  of  the  way  corner  of  South  America. 

The  expedition  was  organized  under  the  direction  of  Profes- 
sor HOLDEN,  of  the  Lick  Observatory,  and  the  instructions  con- 
cerning the  observations  and  other  miscellaneous  work  were 
prepared  by  him. 

We  left  New  York  October  31,  on  the  steamer  "Bermuda," 
Captain  FRASER,  and  after  a  pleasant  voyage  of  two  weeks, 
the  steamer  touching  successively  at  the  islands  of  Santa  Cruz, 
St.  Kitts,  Antigua,  Dominica,  Martinique,  St.  Lucia,  Barba- 
dos, and  Grenada,  we  arrived  at  Port  of  Spain,  Trinidad.  At 
this  place  we  were  detained  ten  days,  awaiting  the  arrival  of 
the  French  steamer  "  Venezuela."  These  stoppages  furnished 
very  welcome  opportunities  for  going  ashore  at  these  very  inter- 
esting tropical  islands,  and  for  making  many  interesting  pho- 
tographic views  of  the  scenery  and  people.  Captain  FRASER 
was  exceedingly  obliging  in  all  ways,  even  to  the  extent  of 
changing  the  ship's  course  temporarily,  to  enable  us  to  make 
instantaneous  views  of  passing  objects  of  interest. 

At  Trinidad  we  were  joined  by  that  veteran  eclipse  observer, 
Mr.  CHARLES  H.  ROCKWELL,  of  Tarrytown,  N.  Y.,  who  came 
from  New  York  via  Colon,  taking  the  "  Venezuela "  at  Mar- 
tinique. Mr.  ROCKWELL  has  probably  observed  more  eclipses, 
transits,  etc.,  than  any  other  living  observer,  and  in  doing  so 
has  visited  all  corners  of  the  globe;  and  as  he  has  been  singu- 
larly successful  in  seeing  the  phenomenon  in  nearly  every 


PLATE  III. 


Report  of  Messrs.  Burnham  and  Schaeberle.       23 


instance,  we  trusted  that  his  good  luck  would  not  be  wanting 
at  the  eventful  moment  in  Cayenne. 

The  voyage  from  Trinidad  to  Cayenne  is  somewhat  barren  of 
pleasant  recollections,  and  fortunately  came  to  an  end  in  about 
six  days,  by  the  arrival  of  the  steamer  at  Cayenne  on  Decem- 
ber 1.  The  boxes  of  instruments  were  taken  ashore  the  next 
day,  and  through  the  courtesy  of  the  Governor  of  the  colony, 
M.  GERVILLE  REACHE,  we  were  given  permission  to  locate  the 
observatory  station  at  a  point  on  the  northern  side  of  the  town, 
occupied  as  a  battery. 

There  were  several  suitable  localities  along  the  shore.  The 
one  selected  had,  however,  a  small  one-story  building  (used  as 
a  boiler  house  for  the  adjoining  hospital),  which  we  found 
would  answer  very  well  as  a  store-room  for  our  subsidiary 
apparatus,  and  for  packing  and  unpacking  our  instruments, 
which  would  have  otherwise  been  exposed  to  the  frequent  rains. 
In  this  same  building  the  dark  room  was  constructed,  and  the 
interior  otherwise  fitted  up  for  office  purposes.  The  rain 
frequently  came  down  in  such  torrents  that  it  forced  its  way 
through  the  crevices  of  the  building  to  such  an  extent  that  the 
concrete  floor  was  scarcely  ever  dry,  and  often  it  was  covered 
with  water  to  the  depth  of  an  inch.  All  those  things  which  it 
was  necessary  to  keep  dry  were  stored  within  the  boiler. 

THE  6^-lNCH  CLARK  EQUATORIAL. 

[See  Plate  III.J 

This  instrument,  belonging  to  the  Lick  Observatory,  has  an 
excellent  object-glass  of  the  usual  form,  by  ALVAN  CLARK  & 
SONS.  The  focal  length  is  shorter  than  usual,  being  only  about 
76  inches.  It  was  mounted  by  WARNER  &  SWASEY,  and  fur- 
nished with  a  driving-clock.  The  pier  is  of  cast-iron,  the  upper 
section  of  which  contains  the  driving-clock.  The  lower  sections 
were  not  taken  to  Cayenne,  their  place  being  supplied  by  two 
pieces  of  timber  firmly  set  in  the  ground,  and  the  instrument 
securely  bolted  to  the  top.  This  made  a  pier  as  good  for  all 
practical  purposes  as  one  of  masonry  or  iron.  A  great  deal  of 
time  was  consumed,  after  the  pier  was  made,  in  getting  the 
instrument  in  working  condition.  The  mounting  is  one  of  the 
complicated  kind,  and  in  the  saturated  atmosphere  of  Cayenne, 


24  Solar  Eclipse  of  December,  1889. 

it  was  impossible  to  keep  anything  in  its  ordinary  condition, 
and  much  labor  was  necessary  to  keep  it  in  suitable  order  for 
use. 

This  instrument,  though  not  intended  for  photographic  work, 
had  been  found  by  Mr.  BARNARD  to  give  good  definition  when 
the  position  of  the  plate  is  a  little  outside  of  the  visual  focus. 
After  the  instrument  was  put  in  position  at  Cayenne,  the  pho- 
tographic focus  was  carefully  determined  by  a  number  of  star 
exposures  on  the  same  plate,  but  at  distances  from  the  visual 
focus  varying  from  each  other  by  perhaps  one  sixteenth  of  an 
inch.  These  experiments  were  sufficiently  repeated  to  give  a 
satisfactory  result.  Before  doing  this,  of  course  the  object-glass 
had  been  carefully  adjusted  to  give  the  best  definition  with  a 
high  power  on  a  selected  test.  It  was  important  at  this  par- 
ticular place,  to  ascertain  the  best  photographic  focus,  as  near 
the  time  of  the  eclipse  as  possible,  since  the  device  for  holding 
the  plate-holder  at  the  eye-end  of  the  telescope  was  made  of 
wood,  and  the  changes  in  it  from  the  excessive  moisture,  at 
times  made  its  exact  position  quite  uncertain.  The  plate-hold- 
ers could  not  be  inserted  at  all  until  portions  of  the  woodwork 
had  been  cut  away,  although  everything  had  been  made  to  work 
smoothly  before  the  instrument  was  shipped. 

The  times  of  exposure  during  totality,  decided  upon  before 
leaving  Mt.  Hamilton,  were  two,  five,  seven,  ten,  and  twenty- 
five  seconds,  the  aperture  being  cut  down  to  three  inches.  This 
programme  was  carried  out,  and  the  several  times  given  as 
accurately  as  it  could  be  done  under  the  circumstances,  'and  in 
order  named.  In  replacing  the  slide  of  the  plate-holder  of  No. 
1,  the  instrument  was  slightly  disturbed,  and  this  motion  is 
shown  on  the  negative,  which  otherwise  is  an  excellent  one, 
but  all  the  others  are  perfectly  sharp.  The  slide  was  drawn, 
and  then  the  exposure  made  by  lifting  a  light  black  velvet  flap 
hinged  above  the  object-glass.  This  was  worked  by  a  string 
from  the  eye-end,  the  flap  returning  to  its  place  by  its  own 
weight  on  letting  go  the  cord.  Nothing  could  be  more  satis- 
factory than  this  plan,  since  with  proper  care  it  could  not 
disturb  the  instrument  in  the  least;  and  the  time  used  in  this 
way  was  reduced  to  the  minimum.  After  these  five  plates 
had  been  exposed,  another  plate  was  put  in  place,  and  the 
exposure  commenced;  but  the  end  of  the  totality  was  reached 


Report  of  Messrs.  Burnham  and  Schaeberle.       25 


a  little  sooner  than  was  expected,  and  the  plate  was  not  cut  off 
until  it  had  received  the  first  flash  of  light.  One  could  hardly 
make  this  fraction  of  a  second  any  shorter,  even  if  it  had  been 
desired  to  expose  a  plate  in  this  way,  but  of  course  the  light 
was  sufficient  to  fog  the  plate  generally,  and  destroy  its  value 
as  a  picture  of  the  corona,  although  it  has  some  points  of  con- 
siderable interest.  During  totality,  the  whole  time  after  begin- 
ning the  exposures  was  given  to  the  photographic  work,  and 
all  that  was  seen  of  the  corona  with  the  eye  was  at  the  first 
instant  of  totality  while  watching  for  the  disappearance  of  the 
last  ray  of  sunlight. 

Shortly  after  third  contact,  a  plate  was  exposed,  the  telescope 
remaining  at  rest,  giving  two  pictures  of  the  Sun  with  an  inter- 
val of  some  minutes  between,  from  which  the  position  of  the 
meridian  could  be  determined. 

THE  DALLMEYER  PHOTOGRAPHIC  TELESCOPE. 

This  instrument  was  borrowed  from  the  U.  S.  Naval  Observa- 
tory, for  the  special  purpose  of  taking  it  to  Cayenne  to  observe 
the  solar  eclipse. 

The  telescope  consists  of  a  short  steel  tube,  into  one  end 
of  which  a  DALLMEYER  portrait  lens  of  six  inches  aperture  is 
screwed;  the  other  end  of  the  tube  contains  the  plate-holder, 
fastened  to  a  short  tube,  which  fits  into  the  main  tube,  and  is 
held  in  position  by  three  small  bolts  passing  through  the  main 
tube,  and  through  slots  in  the  sliding  tube  to  admit  of  an  adjust- 
ment for  focus.  A  small  finder,  about  the  size  of  a  sextant  tele- 
scope, fastened  to  the  side  of  the  tube,  contains  a  set  of  coarse 
lines  in  the  form  of  a  square,  which  serve  to  center  the  Sun's 
image. 

For  the  purpose  of  securing  more  accurate  pointings,  a  tele- 
scope of  nearly  three  feet  focus  was  also  mounted  on  the  main 
tube.  This  finder  was  kindly  loaned  to  the  expedition  by  Mr. 
BARNARD  of  this  Observatory. 

The  tube  is  fastened  to  a  fine  equatorial  mounting  by  ALVAN 
CLARK  &  SONS.  The  clock  work  (BOND'S  escapement)  for  pro- 
ducing the  diurnal  motion  is  attached  to  the  interior  of  the  same 
semi-circular  casting  that  holds  the  polar  axis.  The  connection 
between  the  clock  and  this  axis  is  made  by  means  of  two  steel 
straps  of  the  usual  CLARK  pattern. 


26  Solar  Eclipse  of  December,  1889. 

The  hour  and  declination  axes  are  of  the  usual  form,  the 
circles  reading  to  2s  and  1',  respectively.  The  semi-circular 
piece  which  carries  the  clock  and  the  polar  axis,  can  be  clamped 
at  any  desired  altitude  to  a  close-fitting  casting  which  forms  the 
topmost  piece  of  the  pier;  the  other  parts  of  the  pier  are  two 
sheet-iron  conical  tubes,  which  have  suitable  castings  for  bases. 
To  the  bottom  plate,  the  three  legs  (on  which  the  instrument 
rests)  are  bolted;  an  adjusting  screw,  near  the  extremity  of  each 
leg,  abutting  against  a  circular  plate  placed  on  the  ground,  can 
be  used  for  making  the  finer  changes  in  altitude.  The  adjust- 
ment in  azimuth  is  made  by  twisting  the  conical  tubes  at  the 
joints,  the  bolt  passing  through  the  center  of  the  pier,  which 
serves  to  connect  the  pieces  and  give  the  necessary  rigidity  to 
the  mounting,  being  loosened  for  this  purpose. 

The  observer  stationed  at  this  instrument  called  out  the  time 
of  the  commencement  of  totality  as  determined  by  looking 
through  the  small  finder.  Several  seconds  before  the  final  dis- 
appearance of  the  Sun  the  phenomenon  known  as  Baily's 
Beads  was  quite  marked;  gradually  all  the  bright  points,  with 
the  exception  of  one,  had  disappeared;  this  one  seemed  to  last 
about  two  seconds  and  then  suddenly  vanished.  At  this  instant 
time  was  called.  As  the  primary  object  of  observations  with 
this  instrument  was  to  obtain  the  greatest  possible  extent  of  the 
corona,  even  at  the  sacrifice  of  the  detail  near  the  Sun's  limb, 
the  observer  was  to  make  exposures  of  10s,  15s,  20s,  and  25s, 
either  with  the  full  aperture  of  six  inches,  or  with  a  four-inch 
stop,  as  deemed  best.  The  full  aperture  was  used,  and  the  fol- 
lowing times  given:  5s,  10s,  15s,  20s,  and  23S±.  The  last  was 
to  have  been  25s,  but  the  Sun  reappeared  about  4s  before  the 
expected  time,  so  that  before  the  slide  could  be  pushed  in,  the 
image  of  the  reappearing  limb  of  the  Sun  was  impressed  upon 
the  plates.  It  was  intended  to  make,  if  possible,  one  very  short 
exposure  besides  the  prescribed  ones,  but  the  feat  was  not  accom- 
plished. The  exposures  were  made  by  first  drawing  the  slide 
and  then  uncovering  the  objective.  This  latter  operation  was 
rendered  extremely  easy  by  Mr.  BURNHAM'S  device  of  a  light 
hinged  shutter,  over  the  object-end  of  the  telescope,  which  was 
opened  and  closed  by  means  of  a  string  within  reach  of  the  eye- 
end.  To  diminish  the  sky  glare  a  large  shade  in  the  form  of  a 
hollow  cylinder,  made  of  barrel  hoops  covered  with  black  cloth 


Report  of  Messrs.  Burnham  and  Schaeberle.       27 

and  mounted  on  a  separate  stand,  projected  beyond  the  object- 
ive end  of  the  telescope.  The  full  aperture  of  the  objective,  six 
inches,  was  used.  All  the  negatives  taken  with  this  instrument 
show  that  the  exposure-times  were  very  much  too  long;  the  over- 
exposure  is  so  great  that  the  finer  details  are  not  easily  recog- 
nized. 

During  the  longer  exposures  the  observer  looked  at  the  co- 
rona without  optical  aid.  The  light  was  so  surprisingly  bright 
that  the  belief  in  the  possibility  of  bringing  the  phenomenon 
within  the  reach  of  observation  in  full  sunshine,  when  proper 
precautions  are  taken,  certainly  appeared  to  have  nothing 
absurd  about  it.  Ordinary  terrestrial  objects  were  easily  distin- 
guishable at  apparently  all  distances,  and  on  the  whole  the 
observer  had  the  impression  that  the  illumination  appeared 
much  more  effective  than  that  due  to  the  light  of  the  full  Moon. 
The  impression  produced  on  the  visual  organs  was  much  the 
same  as  that  caused  by  looking  through  a  neutral-tinted  dark 
glass;  terrestrial  objects  were  plainly  visible  and  sharply  defined, 
but  entirely  devoid  of  all  color,  only  the  difference  in  the  degree 
of  colorless  darkness  (if  one  may  be  allowed  the  expression) 
appeared  to  be  the  boundary  line  of  things  seen. 

THE  18-lNCH  REFLECTOR. 

The  optical  part  of  the  reflector  consisted  of  an  18-inch  disc 
of  glass  two  inches  thick,  the  surface  of  which  was  figured  by 
Mr.  SCHAEBERLE  at  Ann  Arbor  in  1880. 

Before  shipping,  the  mirror  was  resilvered.  It  reached 
Cayenne  in  perfect  condition,  and  in  spite  of  the  damp  climate 
the  silvered  surface  retained  its  polish  up  to  the  time  of  our 
departure  from  Cayenne. 

As  we  had  brought  neither  tube  nor  mounting  with  us,  it  was 
necessary  to  construct  these  parts,  as  best  we  could,  upon  the 
ground. 

The  backbone  of  the  tube  consisted  of  two  parallel  pieces  of 
scantling  6  in.  by  6  in.  by  12  ft.,  placed  about  twenty  inches  apart 
and  joined  together  by  inch  boards  placed  diagonally.  To  shut 
out  all  side  lights,  a  number  of  barrel  hoops  were  nailed  to  the 
backbone,  and  the  whole  framework  inclosed  in  a  covering 
made  of  black  cloth,  thus  forming  a  tube  for  the  telescope. 


28  Solar  Eclipse  of  December,  1889. 

The  tub  in  which  the  mirror  was  transported  was  bolted  to  the 
lower  end  of  the  tube,  and  served  as  a  cell  for  the  mirror,  which 
rested  entirely  on  a  cloth  cushion  lining  the  back  and  sides  of 
the  tub. 

The  hour  axis  consisted  of  a  wooden  beam  6  in.  by  6  in.  by  6 
ft.,  having  an  iron  bearing  at  each  extremity,  made  by  rounding 
oif  the  square  head  of  an  iron  bolt  screwed  into  the  wood. 
Heavy  iron  washers  fastened  to  the  rigid  frame-work  of  one  of 
the  cannon  of  the  battery  served  as  boxes  in  which  the  bolt- 
heads  were  free  to  revolve  through  a  small  angle.  The  bearing 
for  the  elevated  end  of  the  hour  axis  was  so  constructed  as  to 
admit  of  an  immediate  change  in  azimuth,  as  it  became  appar- 
ent that  on  account  of  the  unfavorable  weather  the  final  adjust- 
ment in  azimuth  might  possibly  be  delayed  until  the  morning 
of  the  eclipse,  and  such  turned  out  to  be  the  case. 

This  axis  (inclined  5°  to  the  horizon)  was  bolted  to  the  lower 
extremity  of  the  tube,  at  an  angle  of  66-J0. 

The  diurnal  motion  was  communicated  by  means  of  a  screw 
abutting  against  the  upper  end  of  the  tube  and  working  in  two 
nuts  secured  to  a  plank,  which  in  turn  was  supported  by  the 
rigid  castings  of  the  great  cannon. 

The  distance  between  the  screw  and  the  bearings  of  the  hour 
axis  was  made  such  that  one  turn  of  the  screw  caused  a  rota- 
tion of  the  axis  corresponding  to  ten  seconds  of  time. 

As  the  range  of  motion  was  very  small,  it  was  of  course 
necessary  to  limit  all  our  preliminary  work  with  this  rudely 
constructed  instrument  to  that  portion  of  the  sky  which  the 
Sun  was  to  occupy  during  the  two  minutes  of  totality.  For  this 
reason,  as  well  as  the  continual  presence  of  passing  clouds,  the 
efforts  to  determine  the  position  of  the  focal  plane  by  photog- 
raphy, on  the  night  before  the  eclipse,  were  in  vain. 

On  the  morning  of  the  eclipse  our  prospects  of  having  clear 
weather  were  almost  hopeless.  It  had  been  raining  during 
the  night,  and  half  an  hour  before  the  time  of  the  total  phase 
we  were  obliged  to  cover  up  our  instruments  to  protect  them 
from  the  drizzling  rain.  About  twenty  minutes  before  totality 
the  sky  began  to  show  signs  of  clearing  off,  so  that  fifteen 
minutes  before  the  critical  time  everything  was  in  readiness 
with  the  exception  of  the  reflector,  which  required  adjustment 
both  for  position  and  for  focus.  The  only  way  to  focus  the 


Report  of  Messrs.  Burnham  and  Schaeberle.       29 


instrument  was  by  viewing  the  Sun's  image  as  formed  in  the 
plane  which  the  sensitive  plate  was  to  occupy.  The  time  was 
so  very  short  that  there  was  great  danger  of  being  too  late  at 
our  respective  instruments.  Two  minutes  before  the  beginning 
of  the  eclipse,  however,  we  had  made  hasty  and  necessarily 
incomplete  adjustments  of  this  instrument,  and  were  all  ready 
to  make  the  exposures.  There  was  no  dew  on  the  mirror  dur- 
ing the  totality. 

There  were  three  observers  at  this  telescope.  Mr.  ROCKWELL 
agreed  to  count  the  seconds  of  the  chronometer  for  the  whole 
party,  and  also  to  turn  the  screw  giving  the  diurnal  motion  to 
the  telescope.  Mr.  BURKE  inserted  the  plate-holders  and  drew 
the  slide,  while  Mr.  L'HOTE  made  the  exposures  by  removing 
the  great  cap  (made  of  several  thicknesses  of  black  cloth 
stretched  over  a  hoop).  There  were  four  plates  in  two  plate- 
holders,  and  in  order  to  expose  all  of  them  in  the  limited  time, 
the  slide  was  not  entirely  withdrawn  from  the  holder;  all  the 
rays  intercepted  by  the  slide  were  therefore  lost;  besides  this, 
the  image  was  now  formed  by  an  unsymmetrical  cone  of  rays. 
With  the  exception  of  the  8-inch  circular  disk,  held  by  a  half- 
inch  radial  strip  of  wood,  carrying  the  plate-holder,  and  the 
area  (6-inch  by  6-inch)  cut  off  by  the  slide,  the  full  aperture 
of  the  18-inch  mirror  was  used  in  all  the  exposures,  the  dura- 
tions being,  respectively,  1s,  5s,  10s,  and  15s. 

The  unavoidable  irregularities  in  the  turning  of  the  screw 
(Mr.  ROCKWELL  certainly  did  his  work,  as  a  prime  mover, 
almost  to  perfection),  the  errors  of  focal  adjustment,  and  the 
vibrations  resulting  from  the  act  of  drawing  the  slide  from  the 
rather  unstable  plate-holder,  are  shown  in  a  greater  or  less  degree 
in  all  four  negatives. 

OBSERVATIONS  OF  CONTACTS. 

Mr.  ROCKWELL  noted  the  chronometer  times  of  the  second 
and  third  contacts;  the  fourth  contact  was  observed  by  Mr. 
SCHAEBERLE,  with  the  finder  of  the  6-inch  equatorial.  The 
computed  and  observed  local  sidereal  times  are: 


30  Solar  Eclipse  of  December,  1889. 


CONTACTS. 


First. 

Second. 

Third. 

Fourth. 

Computed 

12»>  53m  52s 

13h  56™  11\4 

13h  58'"  13".4 

15»>  9'"  33*.4 

Observed 

Raining  | 

13    56    13 

13    58    11 

15   9    57 

The  chronometer  correction  was  determined  from  a  series  of 
sextant  observations  of  the  Sun  and  stars  made  during  our  stay 
in  Cayenne. 

As  the  position  of  Cayenne  had  previously  been  determined 
with  a  degree  of  accuracy  which  we  could  not  hope  to  attain 
with  a  sextant,  the  only  instrument  available  for  this  purpose, 
the  position  of  our  station  was  referred  directly  to  two  points 
well  determined  by  Admiral  MOUCHEZ.  One  of  these  points  is 
at  the  fort  situated  on  a  rock  several  hundred  feet  above  sea 
level,  at  the  western  limit  of  the  village,  and  about  one  third 
of  a  mile  from  our  station.  The  other  point  is  on  a  large  rock 
out  at  sea,  on  which  a  lighthouse  is  located.  The  name  of  this 
island  is  "Enfant  Perdu."  The  coordinates  are: 


Fort  de  Cayenne,  A=54°  38'  45"    <p=-+4°  56'  24"  I  M 
Enfant  Perdu,        A=54   42    3      <p=+5     2  40  f  * 

The  longitudes  are  reckoned  from  Paris. 

At  the  fort  the  distance  between  the  base  of  the  flagstaff  and 
the  center  of  the  tower  used  for  a  beacon  light  was  measured 
for  a  base  line,  and  found  to  be  51.2  metres,  which,  when  viewed 
from  our  station,  subtended  an  angle  of  4°  50'. 

The  angle  at  the  flagstaff,  between  the  tower  and  our  station, 
was  73°  57',  while  that  between  the  station  and  the  island 
Enfant  Perdu  was  16°  51',  the  station  being  east  of  the  island. 

The  resulting  computed  distance  from  the  station  to  the  fort 
agrees  almost  exactly  with  the  value  obtained  by  scaling  an 
official  map  of  the  place;  taking  this  distance  at  572  metres, 
and  reckoning  the  longitude  from  Greenwich,  the  position  of 
our  station  is  found  to  be: 

Longitude    52°  20'    7"  west. 
Latitude     +4   56  38 

For  computing  the  times  of  contact,  the  provisional  values 
used  were,  respectively,  23"  and  2"  greater  than  the  above  values. 


Report  of  Messrs.  Burn-ham  and  Schaeberle.       31 


THE  ECLIPSE  NEGATIVES. 

The  dry  plates  used  with  the  astronomical  instruments  were 
all  SEED  plates,  sensitometer  26.  These  plates  have  been  used 
exclusively  at  the  Lick  Observatory  for  all  classes  of  subjects, 
and  have  been  found  to  be  uniformly  reliable  and  free  from  all 
defects,  and  with  the  important  property  of  keeping  indefinitely 
without  loss  of  sensitiveness  or  brilliancy  in  the  image.  In 
addition  to  this,  it  is  always  easy  to  make  a  strong  and  "  plucky" 
negative  on  a  plate  of  the  highest  sensitiveness.  These  condi- 
tions are  not  always  found  combined  in  other  plates. 

The  plates  exposed  during  totality  were  leisurely  developed 
in  the  course  of  three  or  four  days  following  the  eclipse.  Every 
precaution  was  taken  to  secure  the  best  results,  so  far  as  devel- 
opment was  concerned.  No  practical  photographer  will  need 
to  be  told  that  this  part  of  the  work  is  second  to  none  in  im- 
portance, and  that  when  everything  else  has  been  properly 
done,  a  careless  or  unskillful  development  of  the  plates  may 
seriously  injure  or  ruin  what  would  otherwise  be  a  valuable 
negative.  The  best  result  can  only  be  secured  by  a  careful 
development  of  each  plate  on  its  own  merits,  and  no  expert 
would  undertake  to  say  in  advance  what  would  be  the  best 
method  for  a  given  exposure.  This  can  be  found  by  cautiously 
starting  the  development  with  a  weak  solution  and  carefully 
watching  the  result,  and  then  modifying  the  proportions  and 
strength  of  the  chemicals  to  suit  each  particular  case.  It 
becomes  then  entirely  a  matter  of  judgment,  derived  from 
practice  and  experience,  and  no  rules,  except  of  the  most  gen- 
eral character,  can  be  given  for  practical  working,  whether  the 
subject  of  the  negative  be  an  eclipse  or  a  landscape. 

The  formula  used  by  Mr.  BUBNHAM  for  several  years,  in  the 
development  of  some  thousands  of  plates,  was  employed  here. 
It  is  made  up  as  follows: 

No.  i. 

Water 16  ounces. 

Pyro 1    ounce. 

Sulphite  of  soda .. 3  ounces. 

No.  2. 
Water _ 32  ounces. 

Sulphite  of  soda 3  ounces. 

Carbonate  of  soda..  ..  4  ounces. 


32  Solar  Eclipse  of  December,   1889. 

This  is  substantially  the  formula  now  given  with  the  SEED 
plates.  The  normal  proportions  for  use  are  one  part  of  No.  1 
to  two  parts  of  No.  2;  two  or  three  drams  of  the  combined 
solution  ordinarily  being  sufficient  to  develop  a  5x7  plate. 
The  proportions  used  of  the  two  solutions  should  be  varied 
to  suit  the  exposure  in  each  case,  and  some  restraining  agent 
used  when  necessary. 

So  far  as  one  could  judge  by  the  times  of  exposure  and  the 
results,  the  development  of  the  eclipse  negatives  was  entirely 
successful.  Each  negative,  after  fixing  and  washing,  was  care- 
fully examined  to  see  whether  any  change  should  be  made  in 
the  manner  of  development;  and  whatever  could  be  learned  in 
this  way  was  made  use  of  in  developing  the  remaining  nega- 
tives. 

The  plates  were  nearly  all  enormously  over-exposed,  and 
particularly  those  made  with  the  DALLMEYER  portrait  lens. 
The  contracted  aperture  of  the  6-inch  telescope  was  r/25,  while 
with  the  DALLMEYER  lens  the  full  opening  used  in  photograph- 
ing was  about  f/6,  giving  for  the  same  time  of  exposure  seven- 
teen times  as  much  light  as  the  CLARK  instrument.  Therefore, 
the  equivalent  exposure  of  the  plate  securing  the  shortest  time 
with  the  portrait  lens  was  at  least  seventeen  times  more  than 
that  of  No.  2  with  the  other  instrument.  The  exposure  of  No. 
2  was  much  too  long  to  give  the  best  detail  of  the  corona  near 
the  Sun;  and  for  all  purposes  of  studying  the  corona,  this  is 
decidedly  better  than  any  of  the  longer  exposures  with  the 
same  instrument.  Judging  from  the  shortest  timed  negatives 
made  on  this  occasion,  the  exposures  with  a  quick  lens,  like  the 
DALLMEYER,  should  have  been  made  with  a  rapid,  instantane- 
ous shutter,  at  least  for  the  best  detail  near  the  Sun. 

It  is  not  intended  by  these  suggestions  to  give  any  directions 
as  to  the  best  plan  of  exposing  plates  on  future  eclipses,  and  no 
practical  photographers  should  be  governed,  or  to  any  great 
extent  influenced,  by  what  other  experts  have  done  at  other 
places  and  at  other  times,  under,  perhaps,  entirely  different 
conditions,  and  using  wholly  different  plates  as  to  sensitive- 
ness and  otherwise.  Any  unusually  good  results  in  this,  as  in 
other  branches  of  photography,  are  likely  to  come  only  from 
the  exercise  of  judgment  of  the  photographer  at  the  time  when 
sound  judgment  can  be  formed — when  the  thing  to  be  done  is 


Report  of  Messrs.  Burnhatn  and  Sckaeberle.        33 

before  him.  Then  he  should  be  in  a  position  to  decide  promptly, 
as  in  taking  any  other  picture,  what,  in  his  judgment,  is  the 
proper  time  to  give;  and  a  portion  of  the  totality,  be  it  short 
or  long,  might  well  be  used  in  this  way.  If  an  expert  in  land- 
scape photography  should  decide  to  make  a  picture  at  a  fixed 
hour  and  minute  on  a  given  future  day,  of  an  ordinary  outdoor 
subject,  and  should  bind  himself  beforehand  to  give  the  plates  an 
unchangeable  time  of  exposure,  it  would  certainly  be  regarded 
by  all  practical  photographers  as  absurd,  although  the  prob- 
abilities might  be  that  one  of  several  trials  would  give  a  passa- 
ble and,  perhaps,  a  good  picture. 

In  another  respect  a  long  exposure  was  unfortunate  on  this 
occasion.  The  air  was  at  all  times  laden  with  moisture,  both 
day  and  night,  and  it  would  be  impossible  to  get  through  such 
a  medium  of  diffused  light  the  slight  differences  between  the 
extreme  corona  and  the  sky,  which  could  be  secured  with  a 
dry  atmosphere  and  a  clear,  dark  sky  beyond,  and  about  the 
right  time  of  exposure.  It  rained  hard  a  few  minutes  before 
totality,  and  although  the  sky  near  the  Sun  was  clear  when 
the  plates  were  exposed,  the  condition  of  things  at  that  time 
was,  doubtless,  apparently  much  more  favorable  than  it  would 
have  appeared  but  for  the  discouraging  outlook  a  short  time 
before.  If  we  could  have  had  a  few  minutes  of  California 
weather  at  the  critical  time,  the  photographic  results  would 
have  been  much  improved. 

To  get  the  greatest  extension  of  the  corona,  the  exposure 
should  be  moderately  short,  and  followed  by  a  long  develop- 
ment in  a  very  weak,  diluted  solution,  but  relatively  strong  in 
the  alkaline  part.  In  other  words,  the  exposure  should  be  such 
that  the  light  of  the  sky  has  no  sensible  effect  on  the  sensitive 
film,  and  the  sky  portions  of  the  plate  after  development  should 
be  nearly  clear  glass.  Then  a  very  slight  excess  of  light  will 
be  apparent  in  the  negative.  The  photographer  has  to  do  in 
this  case  what  he  often  does  in  making  landscape  negatives, 
when  it  is  desirable  to  save  thin,  delicate  clouds.  If  the  ex- 
posure is  a  fraction  of  a  second  too  long,  nearly  every  trace  of 
cloud  forms  is  lost,  and  the  sky  in  the  negative  is  of  substan- 
tially uniform  density  on  every  part  of  the  plate.  Perhaps 
there  is  nothing  in  the  whole  range  of  practical  photography 
more  difficult  to  do  than  to  make  a  first  class  landscape  nega- 
3 


34  Solar  Eclipse  of  December,  1889. 

tive,  and  at  the  same  time  preserve  the  delicate  cloud  grada- 
tions. It  not  only  calls  for  the  exercise  of  the  best  judgment 
of  the  photographer  in  giving  the  correct  time,  but  is  a  test  of 
his  skill  in  developing  the  plate  so  as  to  make  it  a  good  print- 
ing negative. 

Those  who  have  given  long  exposures,  or  advocated  doing 
so,  with  the  object  of  getting  the  greatest  possible  extension  of 
corona  on  the  plate,  must  have  overlooked  the  fact  that  the 
background  of  the  sky  is  luminous,  and  would  soon  fog  a 
sensitive  plate,  if  all  other  light  was  excluded.  The  problem, 
photographically  considered,  has  nothing  to  do  with  the  matter 
of  photographing  a  nebula  on  the  black  ground  of  the  sky  at 
night.  There  the  only  light  which  reaches  the  plate  comes 
from  the  object  to  be  photographed;  and  the  exposure  can  be 
indefinitely  prolonged,  with  the  result  of  constantly  increasing 
the  impression  made  by  the  fainter  nebulous  light.  Undoubt- 
edly the  coronal  light  would  act  on  the  plate  in  the  same  man- 
ner if  all  other  light  could  be  excluded;  and  we  should  have  a 
picture  in  extent  and  detail  far  beyond  the  most  wonderful 
display  ever  seen  with  the  naked  eye.  It  is  not  probable  that 
any  great  advance  will  be  made  in  photographing  the  corona 
until  this  work  is  done  from  some  very  high  elevation.  If  a 
station  could  be  occupied  fifteen  or  twenty  thousand  feet  above 
the  level  of  the  sea,  we  might  expect  some  new  and  important 
results.  It  is  in  such  a  place,  and  perhaps  only  in  such  a  place, 
that  photography  can  be  made  to  do  more  than  any  other 
method  of  observation.  It  is  to  be  hoped  that  the  first  occasion 
for  observing  an  eclipse  from  a  station  of  this  character  will 
be  taken  advantage  of  by  practical  photographers,  who  will  be 
governed  only  by  the  conditions  of  things  as  they  are  at  the 
critical  moment.  Whole  expeditions  could  be  profitably  con- 
densed into  a  single  expert  with  a  portable  photographic 
apparatus,  if  the  locality  made  it  impossible  to  transport  the 
instruments  and  accessories  usually  taken  by  eclipse  parties. 

Before  leaving  Mt.  Hamilton  four  of  the  plates  to  be  used  at 
the  time  of  the  eclipse  had  portions  of  them  exposed  to  the 
light  of  the  so  called  CARCEL  standard  lamp.  The  exposed 
parts  consisted  of  a  row  of  ten  squares  at  one  end  of  the  plates, 
the  first  square  of  each  row  securing  the  light  for  five  seconds, 
the  second  ten  seconds,  the  third  fifteen,  the  fourth  twenty,  and 


Report  of  Messrs.  Burnham  and  Schaeberle.       35 

then  increasing  by  ten  seconds  up  to  the  last  square,  with  eighty 
seconds.  The  other  portions  of  the  plate  were  of  course  pro- 
tected from  the  light.  These  plates  were  exposed  as  Nos.  1 
and  4  with  the  CLARK  telescope,  and  Nos.  1  and  2  with  the 
DALLMEYER  lens. 

Two  other  plates  were  also  exposed  to  the  lamp  in  the  same 
manner,  and  these  were  taken  to  Cayenne  and  brought  back  to 
Mt.  Hamilton  without  being  opened  or  handled  in  any  way. 
Another  set  of  squares  was  then  put  on  each  plate,  and  the 
plates  then  developed  in  the  usual  way.  There  was  a  very 
marked  difference  between  the  two  sets  of  squares  on  the  same 
plate.  This  could  be  explained  in  two  ways  only:  either  some 
change  had  taken  place  in  the  plate  during  its  absence  from 
Mt.  Hamilton,  or  the  light  was  not  the  same  in  both  experi- 
ments. .  It  did  not  seem  probable  that  this  difference  was  due 
to  any  deterioration  or  other  change  in  the  plate,  since  at  least 
eight  or  ten  dozen  of  the  same  kind  of  plates  were  developed 
at  Cayenne,  and  showed  no  evidence  of  any  change.  On  the 
return  voyage  a  good  many  more  were  exposed,  giving  the  most 
satisfactory  results  when  developed  after  returning  to  Mt. 
Hamilton . 

These  squares  were  put  on  the  eclipse  plates  for  the  purpose 
of  comparing  them  with  the  several  portions  of  the  corona  hav- 
ing apparently  the  same  density,  and  obtaining  some  expression 
for  the  light  of  the  corona.  There  are  two  serious  objections 
to  expecting  anything  more  than  the  most  general  conclusions 
by  this  plan. 

In  the  first  place,  as  every  practical  photographer  knows  from 
his  own  experience,  the  density  of  a  photographic  plate  is  not 
proportional  to  the  time.  Within  very  narrow  limits  this  may 
appear  to  hold  practically  good,  but  with  any  considerable  range 
of  light,  or  of  time,  the  density  of  the  film  is  of  but  little  use  in 
measuring  the  actinic  effect.  This  is  apparent  from  the  lamp- 
squares  themselves,  and  particularly  in  those  receiving  the 
longer  times,  and  it  is  very  doubtful  if  any  one  would  be  able 
to  arrange  any  considerable  number  of  them  in  their  proper 
order,  if  they  were  cut  out  and  indiscriminately  mixed  together. 
It  is  very  fortunate  for  nearly  every  practical  application  of 
photography,  that  the  density  of  the  negative  is  not  propor- 
tional to  the  quantity  of  light  received.  If  it  were  not  so,  a 


36  Solar  Eclipse  of  December,  1889. 

large  part  of  the  negatives  made  in  the  every  day  uses  of  the 
camera  would  be  almost  or  quite  worthless,  since  they  would 
consist  largely  of  clear  glass,  representing  the  portions  of  weak- 
est illumination  and  opaque  film  from  the  strongest  lights,  and 
the  prints  would  be  mostly  black  and  white,  the  one  from 
necessary  over-printing  and  the  other  from  equally  unavoidable 
under-printing. 

In  the  second  place,  the  lamp  itself  has  too  many  elements 
of  uncertainty  to  make  even  this  kind  of  comparison  reliable 
for  any  scientific  purpose.  Upon  examining  this  lamp  after 
returning  to  Mt.  Hamilton,  so  many  weak  points  in  its  con- 
struction and  management  were  noticed  that  it  was  thought 
best  to  test  it  to  see  how  well  its  results  would  compare  with 
each  other,  as  well  as  with  ordinary  lights  in  common  use. 
The  lamp  was  used  precisely  as  it  had  been  before,  and  was 
managed  in  the  most  careful,  painstaking  manner.  At  least 
two  sets  of  squares  were  made  on  the  same  plate  on  different 
days,  the  lamp  being  made  to  give  the  same  light  as  nearly  as 
possible  to  the  eye,  and  by  a  strict  observance  of  all  the  instruc- 
tions for  the  use  of  the  lamp.  Without  describing  all  the 
experiments  to  this  end,  the  result,  briefly  stated,  was  that  the 
corresponding  squares  made  with  the  lamp  showed  decided 
differences,  and  occasionally  large  differences;  and  it  appeared 
further  that  the  common  candle,  as  well  as  the  ordinary  lamps, 
could  be  more  safely  relied  upon  to  give  consistent  results. 

There  is  a  further  difficulty  in  measuring  results  by  any 
artificial  standard,  if  such  a  thing  could  be  found,  and  that 
comes  from  the  particular  plate  employed.  It  is  well  known 
that  if  two  different  plates  are  compared  for  relative  sensitive- 
ness, and  one  is  found  to  be  quicker  than  the  other  by  natural 
light,  the  relation  may  be  exactly  reversed  if  artificial  light  is 
employed  for  the  comparison. 

For  the  purpose  of  giving  some  idea,  not  of  the  intensity  of 
the  light  in  different  parts  of  the  corona,  but  of  the  density  of 
the  negative  at  these  points,  we  made  the  following  experiment: 
From  negative  No.  4,  with  the  CLARK  telescope,  five  glass 
positives  were  made,  the  relative  times  of  exposure  being  1,  2, 
4,  and  8.  These  plates  were  developed  at  the  same  time,  and 
a  diagram  made  by  projecting  the  positives  on  a  screen,  and 
carefully  drawing  on  it  the  lines  of  equal  illumination,  the 


0 


PLATE  IV.— Silver  print  of  the  Total  Solar 
Eclipse  of  December,  1889,  from  a  negative 
made  with  the  U.  S.  N.  0.  camera,  by 

J.   M.    SCHAEBERLE. 


Report  of  Messrs.  Burnham  and  Schaeberle.       37 

plates  being  accurately  centered  and  adjusted  in  the  lantern. 
There  would  seem  to  be  no  more  reliable  way  of  determining 
the  contours  of  equal  density,  as  it  is  very  easy  to  draw  these 
lines  either  on  the  positives  or  on  a  sheet  of  paper  after  projec- 
tion, and  make  them  consistent  with  each  other  by  drawing 
them  through  the  same  depth  of  tint.  (See  Figure  1.) 


GENERAL  FEATURES  OF  THE  CORONA. 

The  five  negatives  secured  with  the  CLARK  refractor,  during 
the  total  phase,  all  furnish  most  valuable  data  for  studying  the 
coronal  details.  During  the  exposure  of  the  sixth  plate  the 
Sun  reappeared,  and,  of  course,  fogged  the  plate,  so  that  only 
the  brightest  parts  of  the  corona  show.  The  interesting 
phenomenon  of  Baily's  Beads  is  shown,  both  on  this  negative 
and  the  corresponding  one  taken  with  the  DALLMEYER  lens. 

The  first  of  these  negatives,  Plate  No.  1,  is  of  value  for  deter- 
mining the  actinic  brightness  of  the  general  coronal  areas.  The 
finer  details  are  wanting,  owing  to  a  jarring  of  the  telescope, 
which  caused  a  multiplication  of  the  images  on  the  photo- 
graphic plate. 

Plate  No.  2.  This  is  an  excellent  negative;  the  polar  rays 
are  shown  very  satisfactorily,  as  are  also  the  bifurcations  of 
the  equatorial  wings.  The  serrations  in  the  limb  of  the 
Moon  caused  by  protuberances,  and  the  more  intense  portions  of 
the  inner  corona,  are  most  numerous  in  the  southeast  quadrant. 
These  serrations  are  shown  in  even  greater  numbers  on  Plate 


33  Solar  Eclipse  of  December,  1889. 

No.  1,  but  owing  to  the  shifting  of  the  image  it  was  deemed 
best  to  determine  the  position  angles  of  the  more  prominent 
ones  (tabulated  below)  with  the  aid  of  Plate  No.  2. 

Plate  No.  3.  This  negative  is  considerably  denser  than  No. 
2,  and  some  of  the  features  in  the  wings  are  perhaps  more  sat- 
isfactorily shown.  About  a  dozen  serrations  are  visible. 

Plate  No.  4.  This  plate  is  apparently  the  least  dense  of  any 
taken  with  the  CLARK  instrument;  the  protuberances  are  less 
in  number,  but  in  other  respects  the  negative  is  a  very  satis- 
factory one. 

Plate  No.  5.  This  plate,  as  explained  elsewhere,  was  used 
for  experimental  purposes. 

As  the  various  prints  accompanying  this  report  show  nearly 
all  the  main  features  of  the  coronal  form,  a  more  detailed 
account  of  the  negatives  can  be  dispensed  with,  for  in  any  par- 
ticular investigation  relating  to  the  most  minute  detail  the 
observer  would  naturally  desire  to  consult  either  the  original 
negatives  or  copies  therefrom  made  on  glass,  since  it  appears 
that,  to  a  certain  extent  at  least,  the  same  personality  enters 
into  the  examination  of  a  photograph  that  is  known  to  exist 
in  naked-eye  observations  of  the  corona. 

Of  the  five  negatives  secured  with  the  6-inch  DALLMEYER 
telescope,  the  one  which  received  the  shortest  exposure  (No.  1) 
would  be  the  best,  were  it  not  for  the  fact  that  the  plate  is  more 
or  less  spotted,  and  some  of  these  spots  fall  within  the  limits  of 
the  coronal  outlines.  The  polar  rays  and  the  forked  outlines 
of  the  wings  are  plainly  shown.  The  appearance  of  Plate  No.  2 
plainly  shows  that  it  was  over-exposed;  the  coronal  details  are 
less  plainly  seen  than  they  are  on  No.  1.  Both  of  these  plates 
were  standardized,  and  both  show  signs  of  deterioration,  which 
does  not  seem  to  be  the  case  with  the  other  plates,  which  were 
taken  from  a  fresh  box  opened  the  day  before  the  eclipse. 

Plate  No.  3  was  selected  to  make  a  number  of  positives  on 
glass.  The  silver  prints  contained  in  this  report  were  then 
made  from  negatives  obtained  from  the  best  of  the  glass  posi- 
tives. 

Plate  No.  5  shows  about  the  same  general  extent  as  No.  3, 
but  the  polar  rays  are  almost  obliterated.  In  No.  7  the  short 
narrow  crescent  outline  of  the  reappearing  limb  of  the  Sun  is 
crossed  by  the  same  dark  band  which  is  shown  on  a  similar 


PLATE  V.— Silver  print  of  the  Total  Solar  Eclipse  of  December,  1889, 
from  a  negative  by  J.  M.  SCHAEBEELE,  made  with  a 
reflector  constructed  by  himself. 


Report  of  Messrs.  Burnham  and  Schaeberle.       39 


exposure  made  with  the  CLARK  telescope.  The  general  coronal 
outlines  are  plainly  visible,  although  the  sunlight  badly  fogged 
the  plate. 

Plates  Nos.  4  and  6  were  exposed  after  the  totality,  for  the 
purpose  of  orientation. 

The  first  and  fourth  plates  taken  with  the  reflector  were  not 
marked,  so  that  there  is  a  doubt  as  to  which  is  the  longest  and 
which  the  shortest  exposure.  On  one  of  these  plates  the  con- 
trast between  the  sky  and  corona  is  comparatively  slight,  while 
on  the  other,  the  polar  rays  and  the  protuberances  are  promi- 
nent features.  The  coronal  outlines  can  be  traced  to  a  distance 
of  about  a  diameter  from  the  Sun's  center. 

So  far  as  the  inner  corona  is  concerned,  Plate  No.  2  is  the 
best  of  the  series  obtained  with  this  instrument.  The  polar 
rays,  the  detail  in  the  equatorial  region,  and  the  more  promi- 
nent protuberances,  are  satisfactorily  shown.  No.  3  is  by  far 
the  most  dense  of  the  four/  The  greatest  equatorial  extent  is 
about  three  radii  from  the  Sun's  center. 

The  unstable  mounting  of  the  mirror  and  the  plate-holder, 
and  the  unavoidable  irregularities  in  the  motion  of  the  tele- 
scope, caused  slight  duplications  of  the  coronal  outlines. 

The  silver  prints  given  in  this  report  were  made  from  nega- 
tives, which  are  copies  of  No.  2. 

SERRATIONS  AND  PROTUBERANCES  VISIBLE  ON  PLATE  No.  2— CLARK  TELESCOPE. 


POSITION  ANGLES. 


REMARKS. 


63°.4to   66°.9 

67  .9  to    70  .8 

106  .6  to  108  .2 

109  .0  to  110  .6 
111  .6  to  113  .8  . 
120  .8  to  122  .8  . 
125  .6  to  126  .6  . 
128  .0  to  131  .4  . 
135  .2  to  141  .5 
143  .9  to  149  .6  . 
151  .1  to  152  .4  . 
153  .6  to  156  .3  . 
158  .9  to  162  .2  . 
165  .8  to  169  .9  . 
172  .8  to  173  .8  . 
174  .8  to  176  .2  . 
178  .6  to  180  .6  . 
183  .0  to  184  .5  . 
186  .1  to  190  .2  . 
195  .2  to  197  .0  . 
197  .9  to  199  .3  . 


Deep  indentation.    Prominence,  about  0'.8  high. 
Deep  indentation.     Prominence,  about  0'.4  high. 
Very  strong.    Prominence,  about  I'.l  high,  and  in- 
clined 25°  to  the  normal. 


Prominence,  about  0'.9  high. 
Prominence,  about  0'.6  high. 
Prominence,  about  ^.4  high. 


40  Solar  Eclipse  of  December,  1889. 

ORIENTATION  OF  THE  PRINTS. 

As  the  direction  of  the  meridian  is  not  indicated  on  any  of 
the  accompanying  photographs,  and  as  the  protuberances  are 
not  satisfactorily  shown  on  the  prints,  the  orientation  can  be 
readily  determined  by  means  of  the  heavy  north  polar  ray, 
which  is  shown  on  all  the  prints.  The  center  of  this  nearly 
normal  ray  (the  highest  and  most  westerly  of  the  more  con- 
spicuous north  polar  rays)  has  the  position  angle  4°.8;  the  Sun's 
north  pole  is,  therefore,  2°  to  the  east  of  this  ray.  The  heavy 
arched  boundary  of  the  wing  near  the  south  pole  is  in  the 
southeast  quadrant. 

PHOTOGRAPHIC  PRINTS. 

Accompanying  this  report  are  photographic  prints  from  neg- 
atives by  each  of  the  instruments  used.  To  facilitate  printing, 
and  avoid  the  risk  of  breaking  the  negatives  at  the  printer's, 
duplicate  negatives  were  made  by  contact,  and  those  used  in 
making  the  silver  prints.  In  the  case  of  the  negatives  made 
with  the  6-inch  telescope,  it  was  considered  worth  while  mak- 
ing the  duplicate  printing  negatives  in  such  a  way  as  to  give  in 
the  print  as  much  of  the  outlying  corona  as  possible,  and  at 
the  same  time  not  sacrifice  the  details  of  the  inner  corona, 
which  were  fairly  shown.  It  will  be  understood  that  all  the 
details  shown  in  the  denser  parts  of  the  negatives  would  be 
readily  transferred  to  any  positive  print,  but  the  exposure  in 
printing  either  on  glass  or  paper  would  be  so  long  that  the 
outer  portions  of  the  corona  would  be  greatly  over-printed,  and 
practically  the  extent  of  the  corona  considerably  abridged.  Of 
course  both  extremes  would  be  shown  by  making  two  prints 
from  the  negative,  one  printed  just  long  enough  to  show  the 
less  dense  parts  of  the  corona  at  the  greatest  distance  from 
the  Sun;  and  the  other  printed  long  enough  to  bring  out  the 
coronal  details  in  the  dense  part  of  the  negative,  near  the  Sun. 
For  obvious  reasons  this  was  objectionable,  and  it  was  there- 
fore determined  to  try  the  experiment  of  locally  reducing  one 
of  the  densest  negatives.  For  this  purpose  No.  5  was  selected, 
as  being  the  least  valuable  in  the  event  of  the  experiment  not 
being  as  successful  as  it  was  expected  to  be.  This  was  very 
carefully  reduced  in  the  usual  way.  All  practical  photogra- 


Report  of  Messrs.  Burnham  and  Schaeberle.       41 

phers  have  had  frequent  occasion  to  reduce  small  areas  of  land- 
scape negatives,  in  order  to  make  a  perfect  print,  and  avoid  the 
harsh  whites  which  would  otherwise  be  lacking  in  detail.  The 
result  in  this  case  was  entirely  satisfactory.  The  reduction 
was  of  course  the  greatest  near  the  Sun,  and  gradually  dimin- 
ished until  it  had  no  sensible  effect  near  the  limit  of  the  corona. 
The  negative  then  made  a  print  which  represented,  as  well  as 
possible,  all  that  the  negative  could  be  made  to  show  of  the  form 
of  the  inner  and  outer  corona.  Of  course  this  print  does  not 
represent  the  relative  density  of  the  negative;  in  fact,  it  was 
to  avoid  that,  as  already  stated,  that  the  local  reduction  was 
made.  In  every  other  respect  the  print  is  a  faithful  reproduc- 
tion of  all  that  is  shown  in  the  original  negative.  One  of  the 
shorter  exposures  would  have  shown  the  radial  streamers  far 
better,  and  would  have  included  the  numerous  protuberances, 
which  are  very  marked  in  No.  2.  However,  on  the  whole  it 
was  thought  best  to  make  use  of  this  negative  for  some  of  the 
illustrations.  It  should  be  added  that  a  duplicate  negative, 
enlarged  about  two  diameters,  was  made  from  the  same  original, 
and  some  of  the  copies  of  this  report  will  contain  prints  from 
that,  instead  of  the  unenlarged  negative. 

The  photographic  prints  show  an  extension  of  the  corona  in 
the  longest  direction,  equal  to  about  two  thirds  of  the  Moon's 
diameter.  This  is,  of  course,  less  than  is  shown  by  the  corre- 
sponding negative.  The  reduction  of  negative  No.  5  has  not 
affected  the  weaker  parts  of  the  corona,  but  the  diffused  light 
spread  over  the  whole  plate  from  the  over-exposure  has  so 
fogged  it  that  it  is  difficult  to  say  just  where  the  coronal  light 
ends.  It  is  safe  to  say,  however,  that  it  can  be  fairly  seen  on 
the  plate  for  rather  more  than  one  diameter  of  the  Moon.  The 
extent  of  the  corona  is  shown  better  on  Nos.  2,  3,  and  4,  where 
it  can  be  seen  positively  for  nearly  40'  from  the  Moon's  limb. 
In  negatives  of  this  class  it  is  always  possible  to  suspect  at 
considerable  distances  a  slight  difference  in  the  color  of  the 
film,  but  there  is  great  danger  of  the  imagination  having  too 
much  influence  when  the  direction  of  the  extension  is  known. 
A  good  (if  not  the  best)  test  is  to  place  an  opaque  disc  over 
the  negative,  concentric  with  the  Sun,  and  of  a  diameter  some- 
thing less  than  the  largest  estimate  for  the  corona.  The  outer 
parts  of  the  plate  are  then  well  covered,  leaving  a  ring  of  clear 


42  Solar  Eclipse  of  December, 


glass  about  the  central  disc,  thus  concealing  the  direction  of 
the  sides  of  the  plate,  and  the  coronal  extension  from  the 
observer.  When  this  is  done,  it  will  be  found  that  the  same 
observer  will  place  the  limit  much  nearer  the  center  of  the 
Moon  than  he  would  naturally  do  if  prejudiced  by  having  the 
denser  corona  before  his  eyes.  Of  course  different  observers 
might  not  agree  exactly,  but  the  differences  would  probably 
not  be  very  material.  The  limit  given  should  be  at  a  point 
where  the  effect  of  the  light  is  positive  and  unmistakable,  and 
this  should  be  shown  on  a  lightly  printed  glass  or  paper  pos- 
itive. 

It  would  have  been  possible  to  make  a  drawing  which  should 
combine  the  several  prominent  features  of  the  different  sets  of 
negatives,  but  such  interpretations,  aside  from  the  doubtful 
merit  of  being  artistic  work,  however  carefully  and  conscien- 
tiously made,  are,  of  course,  less  reliable  than  photographs.  All 
certain  and  substantial  features  of  a  negative  can  be  shown 
in  properly  made  silver  prints,  and  this  is  the  best,  if  not  the 
only  evidence,  of  what  it  contains  for  those  who  cannot  examine 
the  negative  personally.  Things  which  cannot  be  made  to 
appear  in  this  way  are  often  much  too  uncertain  to  be  figured 
otherwise;  and  this  applies  equally  to  poor  as  well  as  good 
eclipse  negatives,  as  in  the  former  case  the  uncertainties  are 
more  numerous  and  pronounced.  Of  course  it  will  be  under- 
stood that  a  single  print  cannot  show  all  there  is  in  a  negative, 
for  the  reasons  already  given,  that  the  weaker  portions  will  be 
over-printed  in  bringing  out  the  denser  parts,  and,  therefore, 
two  prints  would  usually  be  necessary. 

PHOTOGRAPHY  IN  THE  TROPICS. 

A  few  suggestions  may  not  be  out  of  place  bearing  upon  the 
practical  side  of  making  photographic  negatives  in  the  damp 
and  hot  regions  of  the  West  Indies  and  the  northern  part  of 
South  America.  The  same  conditions  seem  to  prevail  for  at 
least  twenty  or  thirty  degrees  of  latitude.  Heat  and  dampness 
have  been  considered  to  be  conditions  most  dangerous  to  the 
keeping  of  dry  plates,  and  manufacturers  frequently  caution 
purchasers  to  keep  the  plates  in  a  dry  and  cool  place.  One 
who  has  not  visited  such  a  place  cannot  understand  the  excess- 


Report  of  Messrs.  Burnham  and  Schaeberle.       43 

ive  dampness  which  pervades  everything,  and  the  extreme 
discomfort  produced  by  a  temperature  even  lower  than  90°. 
Clothes  and  shoes  mold  over  night  in  the  sleeping-room,  and 
nothing  ever  seems  to  get  dry,  except  the  new-comer,  whose 
thirst  is  perpetual.  If  these  conditions  had  been  fully  con- 
sidered before  leaving  home,  the  boxes  of  plates  would  have 
been  packed  in  such  a  way  as  to  exclude  them  from  the  outside 
air;  but  this  was  not  done,  and  until  the  plates  had  been 
repeatedly  tested,  it  was  feared  that  they  might  have  received 
some  injury.  As  soon  as  possible  after  arriving  at  Cayenne  a 
dark-room  was  made  for  developing,  and  a  large  number  of 
plates,  which  had  been  exposed  about  Cayenne,  and  before 
reaching  there,  were  developed.  There  was  no  evidence  of  any 
kind  that  the  plates  had  suffered  any  deterioration.  The  nega- 
tives made  and  developed  at  this  time,  though  substantially 
all  instantaneous  exposures,  were  both  creditable  to  the  excel- 
lence of  the  SEED  plates  and  gratifying  to  the  photographer. 
Several  boxes  of  unexposed  plates  were  brought  back,  and 
these,  when  used,  appeared  to  be  in  their  original  condition. 
Some  8x10  plates  exposed  in  Trinidad,  on  the  return  trip  were 
placed  in  a  box  containing  two  unexposed  plates.  When  an 
opporfunity  occurred  to  develop  these  plates,  some  time  after 
returning  to  Mt.  Hamilton,  the  two  unexposed  plates  had  been 
forgotten,  and  one  of  them  was  placed  in  the  developer.  No 
image  appearing,  the  tray  was  placed  on  the  rocker  and  the  de^ 
velopment  was  kept  up  for  at  least  an  hour,  and  perhaps  for  an 
hour  and  a  half.  Then  the  true  state  of  the  case  was  suspected, 
and  the  plate  was  rinsed  and  put  away  to  dry.  Some  days 
later  it  was  put  in  the  camera  and  exposed,  and  as  fine  a  nega- 
tive made  of  the  large  telescope  as  any  one  would  wish  to 
have.  This  certainly  could  not  have  happened  with  either  a 
poor  plate  or  a  damaged  one. 

With  the  chemicals  the  change  was  apparent.  The  sulphite 
of  soda,  though  taken  in  the  original  bottles  as  sealed  by  the 
manufacturer,  had  absorbed  so  much  moisture  that  that  which 
was  originally  a  fine  powder  had  become  a  solid  mass,  which 
could  not  be  dug  out  of  the  bottle  with  a  sharp  steel  implement, 
and  could  only  be  broken  up  by  first  breaking  the  bottle.  The 
carbonate  of  soda  fared  much  the  same  way,  notwithstanding 
the  packages  %were  in  their  original  sealed  condition;  and  the 


44  Solar  Eclipse  of  December,   1889. 

hyposulphite  of  soda  continued  to  absorb  so  much  moisture 
that  there  was  always  in  the  vessel  in  which  it  was  kept  several 
ounces  of  a  saturated  solution.  Of  course  in  such  a  state  the 
usual  quantities  of  carbonate  and  sulphite  of  soda,  weighed  for 
making  up  developer,  became  quite  uncertain  from  the  addi- 
tion of  an  unknown  quantity  of  water;  and  the  best  way  of 
developing  with  the  chemicals  in  this  condition  was  thoroughly 
learned  by  making  a  great  many  exposures  in  and  around  Cay- 
enne, and  experimenting  in  the  development  until  the  best 
proportions  were  found.  In  going  to  a  climate  like  this,  all 
chemicals  which  have  a  tendency  to  absorb  moisture  should  be 
carefully  sealed  with  wax,  or  in  some  other  way  made  air  tight, 
and  particularly  hyposulphite  of  soda,  which  should  be  her- 
metically sealed  in  a  substantial  package;  otherwise  this  chem- 
ical will  become  saturated,  and  the  excess  of  water  will  escape, 
if  possible,  and  perhaps  damage  other  things.  Of  course  plates, 
and  chemicals  which  might  injure  them,  should  never  be  packed 
in  the  same  box.  It  is  always  better  to  take  the  necessary 
developing  materials,  and  develop  the  plates  as  soon  after  expos- 
ure as  possible.  Many  things  will  spoil  an  undeveloped  plate 
which  would  not  injure  a  negative.  This  is  with  reference  to 
the  ordinary  landscape  views. 

For  special  exposures  and  photographic  work  of  particular 
value,  it  goes  without  saying  that  the  plates  should  in  all  cases 
be  developed  on  the  spot.  There  is  nothing  to  lose  by  this 
course,  and  everything  to  gain.  To  say  the  least,  it  is  dangerous 
not  to  do  it;  and  no  one  would  pretend  to  say,  after  developing 
a  flat  and  weak  negative,  which  had  been  transported  a  long 
distance  after  exposure,  that  the  result  would  not  have  been 
entirely  satisfactory  if  carefully  developed  at  the  first. 

THE  ECLIPSE  PARTIES  AT  ILES  DU  SALUT. 

This  is  a  group  of  three  small  islands,  about  twenty-five  miles 
from  Cayenne,  on  the  track  of  vessels  entering  and  leaving  the 
port,  and  is  occupied  as  a  convict  station.  The  English  party 
headed  by  Father  PERRY,  and  the  French  astronomer  Comte  LE 
BAUME,  selected  this  point  as  their  station,  perhaps  for  the  reason 
that  the  totality  would  be  a  few  seconds  longer  than  at  Cayenne. 
These  observers  reached  their  destination  only  two  or  three  days 


Report  of  Messrs.  Burnham  and  Schaeberle.       45 

before  the  eclipse,  and  as  there  was  no  regular  communication 
with  the  islands,  we  did  not  learn  of  their  successful  observations 
until  several  days  after  the  twenty-second.  Comte  LE  BAUME 
came  to  Cayenne,  and  returned  with  us  to  Trinidad  on  the 
steamer.  From  him  we  learned  of  the  serious  illness  of  Father 
PERRY,  and  of  the  hurried  departure  of  the  English  steamer 
for  Demarara  on  the  day  after  the  eclipse. 

It  was  not  until  the  arrival  of  the  "  Venezuela  "  at  Demarara 
on  the  return  voyage  that  we  heard  of  the  lamented  death  of 
this  distinguished  astronomer.  He  carried  out  and  finished  his 
scientific  work,  when  his  physical  condition  was  so  low  that  he 
had  to  be  carried  from  the  shore  to  the  eclipse  instruments,  by 
the  exercise  of  a  power  of  will  which  few  astronomers  could 
manifest  under  such  distressing  circumstances.  A  more  selfish, 
and  less  devoted  and  enthusiastic  astronomer,  would  have 
abandoned  the  object  of  the  expedition,  and  by  promptly  leav- 
ing this  unfortunate  place  perhaps  have  saved  his  life.  Father 
PERRY  was  not  made  of  that  material,  and  evidently  gave  no 
thought  to  personal  conveniences,  when  the  alternative  was  a 
failure  to  secure  the  observations  which  depended  so  much 
upon  his  personal  services.  He  is  entitled  to  be  remembered 
as  one  gf  the  few  great  martyrs  to  astronomical  science. 

CONCLUSION. 

We  are  under  many  obligations  to  his  Excellency,  GERVILLE 
REACHE,  the  Governor  of  the  province,  for  every  courtesy  and 
assistance  within  his  power  during  our  entire  stay. .  Nothing 
was  wanting  on  his  part  to  make  our  visit  to  Cayenne  pleasant, 
and  the  special  object  of  the  trip  a  success.  The  American 
Consul,  Mr.  L.  WACOGNE,  was  untiring  in  his  efforts  to  assist 
us,  and  freely  gave  a  considerable  part  of  his  time  in  making 
necessary  arrangements  to  carry  out  the  work.  We  are  deeply 
indebted  to  these  gentlemen  for  their  kindness,  courtesy,  and 
material  help,  and  they  are  entitled  to  a  liberal  share  of  what- 
ever credit  may  be  due  for  the  success  of  the  observations. 

We  are  also  specially  indebted  to  Mr.  GEORGE  H.  CHRISTALL, 
of  New  York  City,  the  representative  of  the  steamship  line 
between  New  York  and  Trinidad,  for  personally  attending  to 
many  details  connected  with  the  receiving  of  the  instruments 


46  Solar  Eclipse  of  December,  1889. 

in  New  York,  storing  them,  and  shipping  them,  and  again  look- 
ing after  them  upon  our  return.  Mr.  CHRISTALL  gave  us  much 
valuable  information  concerning  the  places  we  were  to  visit,  and 
generally  aided  us  in  every  way  in  his  power. 

We  left  Cayenne  January  3,  on  the  "  Venezuela,"  reaching 
Trinidad  on  the  eighth.  We  were  detained  three  or  four  days 
at  Port-of-Spain,  awaiting  the  sailing  of  the  American  steamer, 
and  then  left  for  New  York  direct,  hy  the  "Cohan,"  Capt. 
ROBERT  FRASER,  where  we  arrived  011  January  19. 

•  S.  W.  BURNHAM. 

J.    M.    SCHAEBERLE. 


PLATE  VI. 


'   '      •'''•  '  •'i'niMni    /J,., 

///  .«• 


Plate    VII. — Models    illustrating  the  method  of  formation  of 

the  Polar  Rays. 


A  Mechanical  Theory  of  the  Solar  Corona.       47 


A    MECHANICAL   THEORY    OF    THE    SOLAR 
CORONA. 

By   J.    M.    SCHAEBERLE. 


The  essential  principles  which  lie  at  the  foundation  of  the 
theory  here  advanced  were  first  published  last  spring  in  a  short 
note  entitled  "A  Mechanical  Theory  of  the  Solar  Corona." 
(Publications,  A.  S.  P.,  No,  7;  Mon.  Not.,  R.  A.  S.,  Vol.  4,  p. 
372.)  One  year  previous  to  this  time  (in  February,  1889),  I 
expressed  my  belief  to  Professor  HOLDEN  and  other  astrono- 
mers at  this  Observatory,  that  the  coronal  form  was  produced 
by  streams  of  matter  ejected  from  the  lower  latitudes  of  the 
Sun.  At  the  time  Professor  HOLDEN  desired  me  to  work  up  the 
subject,  and  offered  to  give  me  any  assistance  in  his  power; 
but  as  I  had  not  given  much  attention  to  solar  observation, 
and  was  still  less  familiar  with  the  physical  researches  of  those 
who  made  the  Sun  a  special  study,  I  did  not  deem  the  subject 
a  proper  one  for  me  to  cope  with  at  that  time,  although  I 
intended  to  attack  the  problem  later  on. 

Through  the  liberality  of  Colonel  CROCKER,  who  offered  to 
bear  the  expense  of  an  expedition  to  South  America,  to  observe 
the  solar  eclipse  of  December  21-22,  this  problem  of  the  solar 
corona  was  to  rivet  my  attention  sooner  than  I  had  anticipated. 

The  highly  satisfactory  results  secured  by  the  Lick  Observa- 
tory party,  consisting  of  S.  W.  BURNHAM  and  J.  M.  SCHAEBERLE, 
at  Cayenne,  South  America,  were  such  that  after  the  develop- 
ment of  our  plates  the  views  which  I  had  held  for  nearly  a  year 
were  very  much  strengthened. 

By  the  time  we  again  reached  the  Lick  Observatory  the  super- 
structure of  the  present  theory  was  built,  and  it  only  required 
the  finishing  touches  relating  to  the  more  minute  details  of  the 
corona,  and  a  comparison  with  published  observations,  to  bring 
the  matter  to  its  present  shape. 

In  what  follows  I  shall  present  the  theoretical  investigations 
in  as  simple  and  brief  a  manner  as  possible. 


48       A  Mechanical  Theory  of  the  Solar  Corona. 

Three  well  known  facts  serve  as  a  basis  on  which  the  whole 
theory  rests.  They  are: 

1.  The  eruptions  of  the  Sun's  surface  are  most  active  and 
numerous  in  the  spot-zones. 

2.  The  Sun  rotates  about  an  axis  passing  through  its  center. 

3.  This  axis  is  inclined  to  the  plane  of  the  Earth's  orbit  at  an 
angle  of  about  82%°. 

As  the  present  theory  also  enables  one  to  reproduce,  graph- 
ically, practically  all  the  phenomena  observed  during  a  total 
eclipse  of  the  Sun,  and  as  the  graphical  construction  is  in  strict 
accordance  with  known  mechanical  laws,  the  following  brief 
statement  of  the  theory  may  be  properly  made  here: 

The  theoretical  corona  is  caused  by  light  emitted  and  reflected 
from  streams  of  matter  ejected  from  the  Sun,  by  forces  which,  in 
general,  act  along  lines  normal  to  the  surface  of  the  Sun ;  these 
forces  are  most  active  near  the  center  of  each  Sun-spot  zone. 

Owing  to  the  rotation  of  the  Sun,  the  streams  of  matter  will 
not  lie  along  normals,  since  the  angular  velocity  of  different 
portions  of  a  stream  grows  less  as  the  distance  from  the  Sun 
increases;  in  other  words,  the  streams  are  of  double  curvature. 
Each  individual  particle  of  the  stream,  however,  describes  a 
portion  of  a  conic  section,  which  is  a  very  elongated  ellipse,  so 
long  as  the  initial  velocity  is  less  than  three  hundred  and 
eighty-three  miles  per  second  (assuming  that  the  Sun's  atmos- 
phere, as  shown  by  various  observations,  is  exceedingly  rare). 

Certain  variations  in  the  type  of  the  corona  admit  of  an  ex- 
ceedingly simple  explanation,  being  principally  due  to  the 
change  in  the  position  of  the  observer  with  reference  to  the 
plane  of  the  Sun's  equator.  According  as  the  observer  is  above, 
below,  or  in  the  plane  of  the  Sun's  equator,  the  perspective  over- 
lapping and  interlacing  of  the  streamers  cause  the  observed 
apparent  variations  in  the  type  of  the  corona. 

The  general  direction  in  which  these  ejective  forces  act  will 
be  along  radii.  There  may,  of  course,  be  numerous  particular 
exceptions  to  this  general  direction. 

Similarly,  since  observation  shows  that  certain  solar  motions 
are  apparently  confined  to  special  regions,  which  are  symmet- 
rically situated  with  reference  to  the  axis  of  rotation  of  the  Sun, 
we  are  evidently  justified  in  assuming  that  the  forces  which 
cause  these  motions  are,  in  general,  uniformly  distributed 


By  J.  M.  Schaeberle.  49 

around  each  circle  of  latitude,  since  there  is  no  a  priori  reason 
why,  in  a  highly  heated  rotating  mass  of  matter,  the  solar  ac- 
tivity should  be  confined  to  any  particular  circles  of  longitude. 
There  may,  of  course,  be  particular  exceptions  to  a  uniform  dis- 
tribution of  the  forces. 

As  the  exact  nature  of  the  atmosphere  surrounding  the  Sun 
is  unknown,  and  as  its  extreme  rarity  has  been  demonstrated 
by  various  observations,*  the  heliocentric  motions  of  all  parti- 
cles exterior  to  the  Sun's  visible  surface  will  be  considered  to 
be  unimpeded  by  solar  atmospheric  resistances. 

What  precedes  may  be  taken  to  be  a  complete  statement  of 
the  general  features  of  the  mechanical  theory  of  the  corona. 
In  order  to  compare  it  with  observation  it  will  be  necessary  to 

*NOTES. — With  reference  to  the  views  of  solar  physicists  on  the  subject  of  the 
Sun's  atmosphere,  I  quote  a  few  paragraphs  giving  the  most  recent  conclu- 
sions : 

Professor  YOUNG,  in  his  General  Astronomy,  says:  "The  corona  cannot  be  a 
true  '  solar  atmosphere '  in  any  strict  sense  of  the  word.  No  gaseous  envelope 
in  any  way  analogous  to  the  earth's  atmosphere  could  possibly  exist  there  in 
gravitational  equilibrium  under  the  solar  conditions  of  pressure  and  tempera- 
ture. The  corona  is  probably  a  phenomenon  due  somehow  to  the  intense 
activity  of  the  forces  there  at  work;  meteoric  matter,  cometic  matter,  matter 
ejected  from  the  Sun,  are  all  concerned. 

"  That  this  matter  is  inconceivably  rare  is  evident  from  the  fact  that  in  sev- 
eral cases  comets  have  passed  directly  through  the  corona  without  experiencing 
the  least  perceptible  disturbance  of  their  motions.  It  is  altogether  probable 
that  at  a  very  few  thousand  miles  above  the  Sun's  surface,  its  density  becomes 
far  less  than  that  of  the  best  vacuum  we  can  make  in  an  electric  lamp." 

The  following  paragraphs  are  from  Mr.  KEELER'S  Report  on  the  Solar  Eclipse 
of  January  1, 1889  (published  by  the  Lick  Observatory): 

"  Spectroscopic  observation  furnishes  us  with  many  facts  which  cannot  be 
reconciled  with  the  theory  of  an  extensive  solar  atmosphere.  Two  of  the  most 
important  objections  drawn  from  this  source  are  given  below;  the  first  has 
long  been  recognized  as  especially  perplexing : 

"  (1)  The  pressure  at  the  surface  of  the  chromosphere  is  shown  by  the  spec- 
troscope not  to  exceed  that  of  a  few  millimetres  of  mercury,  and  this  we  must 
accept  as  the  pressure  due  to  an  atmosphere  from  half  a  million  to  a  million 
of  miles  deep,  notwithstanding  the  fact  that  the  force  of  gravity  is  twenty- 
seven  times  as  great  at  the  surface  of  the  Sun  as  at  the  surface  of  the  Earth. 

"(2)  According  to  theory,  as  well. as  observation,  the  upper  limits  of  the 
gaseous  envelopes  of  the  Sun  ought  to  be  ordered  according  to  their  densities. 
The  material  which  produces  the  1474  K  line,  and  which  may  always  be  seen 
in  the  chromosphere  spectrum,  is,  according  to  this  criterion,  as  unmistakably 
denser  than  hydrogen  as  is  magnesium  vapor  or  iron  vapor;  but  if  we  accept 
the  coronal  spectrum  as  evidence  of  the  existence  of  an  atmosphere,  we  are, 
by  exactly  the  same  principle,  driven  to  the  same  conclusion  that  the  1474  K 
material  is  far  less  dense  than  hydrogen.  The  contradiction  could  not  be 
more  abrupt  and  inexplicable." — HASTINGS. 

4 


50        A  Mechanical  Theory  of  the  Solar  Corona, 

deduce  the  laws  which  govern  the  appearances  of  a  typical 
corona  produced  by  solar  eruptions  of  the  character  already  de- 
scribed. For  convenience,  I  have  made  no  distinction  between 
the  real  and  these  theoretical  solar  phenomena;  it  should 
therefore  be  borne  in  mind  that  in  the  discussion  for  deducing 
the  laws  of  coronal  phenomena  this  theoretical  corona  is  always 
the  one  referred  to. 

We  shall  first  inquire  into  the  form  of  the  trajectory  of  a 
particle  ejected  from  the  Sun  by  a  force  sufficient  to  remove  it 
one  or  more  diameters  from  the  Sun's  surface. 

If  there  were  no  motion  of  rotation,  all  particles  ejected  from 
a  given  point  on  the  Sun's  surface  would,  in  general,  lie  along  a 
normal  passing  through  this  point.  The  rotation  of  the  Sun, 
however,  introduces  other  forces,  the  resultant  of  which  can, 
without  appreciable  error,  be  regarded  as  acting  at  right  angles 
to  both  the  axis  of  rotation  and  the  line  along  which  the 
ejective  force  acts. 

In  considering  the  motion  of  an  ejected  particle: 

Let  T0  denote  the  time  of  one  rotation  of  the  Sun  (in  latitude  g>). 
Let  R0  denote  the  radius  of  the  Sun. 

Let  R   denote  the  radius-vector  of  the  ejected  particle  at  the  time  t. 
Let  <p  denote  the  heliocentric  latitude  of  the  point  of  ejection. 
Let  Vi  denote  the  linear  velocity  of  the  particle  due  to  the  Sun's  rotation. 
Let  i)2  denote  the  velocity  of  ejection. 
Let  V  denote  the  resultant  initial  velocity  of  the  particle. 
Let  1})    denote  the  angle  between  a  normal  at  the  point  of  ejection  and  the 
actual  initial  direction  of  motion. 

The  following  expressions  give  the  relations  existing  between 
the  quantities  which  determine  the  subsequent  motion: 


If  TQ  is  expressed  in  seconds,  v1  is  the  distance  described  in 
one  second  of  time. 


V 


(2) 
(3) 


It  is  evident  that  so  long  as  the  line  of  action  of  the  ejective 
force  is  along  a  normal,  any  transverse  force,  however  great  or 
small,  will  at  once  determine  the  position  of  the  plane  in  which 


By  J.  M.  Schaeberle.  51 

the  subsequent  motion  of  the  particle  lies,  since  the  lines  of 
action  of  both  forces  must  lie  in  this  plane.  If  .there  are  sev- 
eral transverse  forces,  the  plane  of  motion  must  contain  a 
normal  through  the  point  of  ejection  and  the  resultant  of  the 
several  transverse  forces. 

The  value  of  vl  is  dependent  only  on  q>}  and  can  therefore  be 
determined  accurately.  If  we  assign  different  values  to  v2  we 
can  evidently  compute  all  the  elements  of  the  several  orbits 
which  would  be  described  corresponding  to  different  initial 
velocities,  since  we  also  know  the  mass  and  radius  of  the  Sun. 
In  other  words,  we  have  given  the  radius-vector  and  the  veloc- 
ity and  direction  of  motion  of  a  particle  at  a  given  instant  of 
time  to  find  all  the  elements  of  the  orbit  described,  the  central 
force  being  known. 

Let  a  denote  the  semi-major  axis  of  the  eclipse  described. 
Let  K2  denote  the  mass  of  the  Sun. 

(The  value  of  Kz  is  such  that  if  the  Sun  acts  on  a  stationary 
material  particle  free  to  move,  at  a  distance  equal  to  the  Earth's 
mean  distance  from  the  Sun,  the  velocity  of  the  particle  at  the 

irri>  v 

end  of  one  second  of  time  will  be  equal  to  24x60x60  ) 
The  general  equation  for  undisturbed  motion  is: 

V^K>  (f-i)  (4) 

From  which  we  can  evidently  find  a. 

We  next  obtain  the  periodic  time  t  from  the  familiar  expres- 


-  (5) 

The  eccentricity  e  can  be  found  as  follows: 

Let  R  and  R  denote  the  distances  of  the  particle  from  the 
two  foci  of  the  eclipse,  then  for  R  =  R0  the  angle  included  be- 
tween R  and  R'  is  always  equal  to  180  —  2^,  so  that  we  can  at 
once  write: 


e=  -/  RJ  +  R'2  —  2  R0  R'  cos  (180°  —  2  $)  (6) 

from  which  £  is  readily  found. 

To  determine  the  inclination  of  the  plane  of  the  orbit  to  the 
Sun's  equator,  we  have  given  a  point  (the  Sun's  center)  and  a 
line  (the  actual  path  of  the  particle  —  the  projection  of  this  path 
on  the  Sun's  surface  at  the  instant  of  ejection  being  nearly  parallel 
to  the  equator)  through  which  the  plane  of  the  orbit  must  pass. 


52        A  Mechanical  Theory  of  the  Solar  Corona, 


The  inclination  of  the  plane  must  evidently  always  be  nearly 

the  same  as  the  latitude  of  the  point  where  the  particle  is  ejected. 

I  have  computed  the  paths  of  particles  for  different  velocities 

of  ejection  in  a  mean  latitude  of  15°.     The  elements  are  given 

in  the  following  table: 

TABLE  I. 


Initial  Velocity 
of   an  Ejected 
Particle=V. 

Angle    between 
the  Normal  at 
the    Point    of 

Semi-Major  Axis 
of  the  Orbit=a 

Periodic     Time 
of    the    Parti- 
clc==£. 

£ 

Ejection    and 

the  Initial  Di- 

Miles per  second. 

rection  of  Mo- 
tion;^;. 

Radius  of  Sun=l 

Expressed   in 
Days. 

Eccentricity. 

219.1 

0°.318 

0.75 

0.075 

0.9933 

269.2 

.259 

1.00 

.116                     .9950 

311.3 

.225 

1.50 

.214 

.9967 

330.3 

.212 

2.00 

.329 

.9975 

348.3 

.201 

3.00 

.604 

.9983 

357.0 

.196 

4.00 

.930 

.9987 

362.1 

.193 

5.00 

1.300 

.9989 

372.2 

.188 

10.00 

3.678 

.9995 

377.0 

.185 

20.00 

8.263 

.9997 

379.5 

.185 

40.00 

29.42 

.999-f 

379.7 

.185 

80.00 

83.22 

.999+ 

382.0 

.184 

Infinity 

Infinity 

1.000 

Apparent  motions  corresponding  to  component  velocities  of 
two  hundred  and  fifty  miles  per  second  (the  actual  velocity  is, 
as  a  rule,  always  greater  than  the  observed)  are  not  infre- 
quently observed  in  solar  protuberances.  (See  Young's  General 
Astronomy,  page  208.)  It  does  not,  however,  follow  that  the 
forces  producing  these  motions  must  be  correspondingly  great, 
for  if: 

v-S-        "•;•;• < 

(in  which  F,  V,  and  M  are  respectively  the  moving  force,  the 
maximum  velocity  generated,  and  the  mass  moved),  then  for  a 
constant  force  F  the  velocity  V  will  increase  as  the  mass  M 
diminishes,  and  as  the  resistance  to  motion  is  to  be  considered 
zero,  the  volume  corresponding  to  a  given  mass  may  be  either 
great  or  small  without  affecting  the  velocity. 

The  above  elements  show  that  the  theoretical  orbit  will 
always  be  a  very  elongated  ellipse,  the  perihelion  point  being 
near  the  Sun's  center  and  having  a  longitude  nearly  180°  dif- 
ferent from  the  longitude  of  the  point  of  ejection,  while  the 
nodal  points  Will  always  be  90°  and  270°  from  the  theoretical 
perihelion,  and  within  less  than  a  score  of  miles  of  the  Sun's 
center. 


By  J.  M.  Schaeberle. 


53 


Let  us  now  consider  the  circumstances  of  motion  of  a  series  of 
particles  ejected  from  the  same  point  on  the  Sun's  surface  following 
each  other  so  as  to  form  a  continuous  stream.  The  angular  velocity 
of  each  particle  as  it  leaves  the  Sun's  surface  will  be  the  same 
as  that  of  the  Sun,  but  as  the  radius- vector  of  the  particle 
increases  the  angular  velocity  decreases  according  to  rigorous 
mechanical  laws.  Therefore,  while  each  particle  may  be  con- 
sidered as  describing  an  independent  orbit,  the  curve  formed 
by  the  stream  will  not  be  a  conic  section,  but  a  helix,  which, 
so  long  as  the  latitude  of  the  base  of  the  stream  is  not  zero, 
will  necessarily  be  of  double  curvature.  As  all  the  particles 
causing  the  visible  coronal  outlines  are  within  a  few  diameters 
of  the  Sun,  we  can,  without  appreciable  error,  consider  a  given 
stream  as  lying  in  one  plane.  For  simplicity  in  the  discussion, 
a  parabolic  velocity  will  be  assumed  for  all  streams: 

Let  GOO  denote  the  true  anomaly  for  a  radius-vector  R0  and  time  to. 

Let  GO  denote  the  true  anomaly  for  a  radius-vector  R  and  time  t. 

Let  T  denote  time  of  the  theoretical  perihelion  passage. 

Let  t  denote  the  time  corresponding  to  R  and  GO. 

Let  6  denote  the  angle  turned  through  by  the  Sun  during  the  time  (t— to). 

With  the  well  known  relations  which  exist  between  (t — T )  and 
GO  in  the  case  of  parabolic  motion,  the  results  given  below  are 
readily  obtained.  The  angle  6  is  zero  at  the  instant  t0  when 
GO  =  GOO  and  R  =  R0.  Both  6  and  GO — GOO  are  measured  from  the 
fixed  heliocentric  direction  in  space  which  the  origin  of  the 
stream  has  at  the  instant  t0.  The  angle  which  a  line  drawn 
from  the  base  of  the  stream  to. any  point  in  the  stream  makes 
with  a  normal  through  this  base,  will  be  called  /. 

TABLE  II. 


Radius-Vector   of 
the  Particle=.ft= 

1.0.      . 

2.0. 

3.0. 

4.0. 

5.0. 

6.0. 

180°—  GO 

0°  22'.  1 

0°  15'.6 

0°  12'.  8 

0°  ll'.O 

0°  9'.9 

0°  9'.0 

t—T  . 

04.009 

Od.025 

0!.045 

04.070 

Od.097 

04.128 

t  —  tn 

0^000 

Od.016 

04.036 

Od.061 

04.088 

Od.119 

Grt  —  ft?0  .  

O'.O 

6'.5 

S'.S 

ii'.i 

12'.2 

13M 

e......  : 

o°.o 

0°.2 

0°.5 

0°.8 

1°.2 

1°.6 

7    ._  

0°.2 

0°.5 

0°.9 

1°.3 

1°.8 

54        A  Mechanical  Theory  of  the  Solar  Corona, 


TABLE  II — Continued. 


Radius-  Vector  of  the  Parti  - 

Cle=£= 

7.0. 

8.0. 

10.0. 

20.0. 

40.0. 

180°—  G3 

0°  8'.3 

0°  ?.8 

0°  7'.0 

0°  4'.9 

0°  3'.5 

t—T 

OU62 

OU98 

Oa.278 

Qd.782 

2<U8 

t  —  t 

Od.153 

OU89 

01.269 

ft*.  773 

2<U7 

CO  GO 

13'.  7 

14'.  3 

15M 

17'.2 

18'.6 

Q 

2°.l 

2°.  6 

I 

2°  3 

2°.  8 

The  equation  which  fairly  represents  the  relation  between  R 
and  /,  I  find  to  be  the  following: 

I  =  -hIP  +  lR-\,  (7) 

/  being  expressed  in  degrees  of  arc  and  the  unit  of  R  being  a 
radius  of  the  Sun. 

For  discussing  the  curve  represented  by  the  above  equation, 
it  will  be  more  convenient  to  take  the  origin  on  the  Sun's  sur- 
face at  the  base  of  the  stream  and  refer  the  curve  to  a  normal 
through  this  origin. 

For  all  points  in  any  stream  visible  during  an  eclipse  we  can 
without  sensible  error  write: 

P  =  R-l,  (8) 

p  being  the  distance  from  any  point  in  the  stream  to  the  Sun's 
surface. 

Equation  (7)  now  becomes 

/=*(/»  +  !)•  +  *  P.  (9) 

Since  for  our  limits  the  angle  /  will  always  be  small,  the  in- 
clination r  of  the  curve,  at  any  point,  to  a  normal  through  the 
origin  will  be  given  by  the  differential  expression 

r=P~+i=^P(p  +  i)+kP  +  i,         (10) 

r  being  expressed  in  degrees  of  arc. 

With  the  aid  of  this  equation  we  obtain  the  following  incli- 
nations P  for  the  corresponding  values  of  p,  the  values  of  / 
being  taken  from  Table  II: 


By  J.  M.  Schaeberle. 


55 


TABLE  III. 


1.0 

0°.5 

2.0 

1.2 

3.0 

2.0 

4.0 

3.0 

'5.0 

4.1 

6.0 

5.4 

7.0 

6.8 

If  fi  denotes  the  Earth's  angular  distance  above  or  below  the 
plane  of  the  Sun's  equator  at  the  time  of  observation,  a  streamer 
in  latitude  cp,  in  order  to  be  just  visible  at  either  pole  of  the  Sun, 
must  have  a  length  p0  given  by  the  equation: 


sn    <± 


— 1 


(11) 


The  values  of  p0  for  the  two  latitudes  15°  and  30°,  and  for 
particular  values  of  /?,  are  given  in  the  following  table  (re- 
ferred to  the  nearer  hemisphere) : 


TABLE  IV. 


Latitude  on  the  ®=<p. 

Angular    Distance   of   the 
Earth  above  the  Plane  of 
the  O's  Equator=#. 

Length  of  a  Streamer  from 
the  Sun,  which  will  just 
be    Visible    at    the    o's 
Pole=/J0. 

±15° 

=F  7°.25 

1.64 

±15 

-4-  7.25 

6.42 

+15 

0. 

2.86 

±80 

0. 

1.00 

+30 

=F  7.25 

0.65 

±30 

-4-  7.25 

1.59 

A  simple  way  to  represent  graphically  the  apparent  changes 
in  the  form  and  position  of  a  streamer,  due  to  the  change  in 
the  position  of  the  Earth  and  to  the  rotation  of  the  Sun,  is  to 
construct  a  model  of  a  single  streamer  issuing  from  a  sphere 
and  to  project  the  streamer  on  a  plane  surface  by  parallel  rays 
of  light.  If  the  sphere  be  rotated,  and  the  inclination  of  the 
axis  of  rotation  varied  between  the  proper  limits  (correspond- 
ing to  the  positions  of  the  Earth  at  different  seasons  of  the 
year),  all  the  peculiarities  of  the  appearances  of  the  coronal 
streamer  can  be  reproduced  and  studied  at  leisure. 

In  order  to  sh6w  more  forcibly  the  varying  form  and  position 


56        A  Mechanical  Theory  of  the  Solar  Corona, 

of  a  streamer  in  projection,  I  have  exaggerated  the  curvature  in 
the  model  used  for  obtaining  the  outline  given  in  Plate  VIII. 

The  streamer  represented  by  a  wire  rod  was  made  to  issue 
from  a  latitude  of  about  15°,  and  to  have  such  a  length  that  in 
projection  it  was  just  visible  at  the  pole  for  ft  =  0°.  A  longer 
streamer  would  have  necessitated  the  use  of  a  smaller  scale. 

The  figures  at  the  extremities  of  the  lines  representing  the 
streamers  correspond  to  the  number  of  days  elapsed  since  the 
base  of  the  streamer  was  on  the  central  meridian  of  the  nearer 
hemisphere. 

Fig.  1,  of  Plate  VIII.,  corresponds  to  an  inclination  ft  =  0, 
Fig.  2  to  the  time  when  the  Earth  is  near  its  maximum  dis- 
tance below  the  plane  of  the  Sun's  equator,  and  Fig.  3  to  the 
time  when  the  Earth  is  near  its  maximum  distance  above  the 
same  plane. 

The  general  outlines  of  the  figures  on  Plate  VIII.  are  evidently 
the  same  as  would  be  produced  by  a  series  of  equidistant 
streamers  issuing  from  a  single  latitude  only. 

If  now  the  streamers  issue  from  different  latitudes  within 
the  limits  of  the  Sun-spot  zones,  coronal  forms  similar  to  those 
shown  on  Plate  VI.  (which  are  made  from  an  actual  model,  as 
described  on  the  plate  itself)  will  be  produced.  In  a  typical 
corona  the  mean  latitude  of  the  zone  from  which  the  streamers  issue 
will  always  be  the  same  as  the  latitude  of  the  densest  and  most 
extended  portion  of  the  coronal  outlines.  A  necessary  consequence 
of  the  perspective  overlapping  of  these  streamers  is  the  production 
of  luminous  rays  which,  in  a  typical  corona,  incline  away  from  the 
adjacent  poles,  as  will  be  demonstrated  further  on. 

A  crucial  test  of  this  or  any  other  theory  of  the  corona  is 
afforded  by  the  appearance  and  behavior  of  these  so  called 
"polar  rays."  If  they  really  originate  at  or  very  near  the  Sun's 
polar  regions,  the  laws  governing  their  appearance  must  be 
sought  for  in  the  physics  of  the  Sun  itself.  If,  however,  the 
present  conception  of  their  origin  is  the  true  one,  they  are 
mainly  due  to  a  series  of  apparent  intersections  of  streamers 
from  the  Sun's  equatorial  region,  projected  by  perspective  above 
or  below  the  poles;  that  is,  the  polar  rays  which  we  see  in  any 
corona  have  no  objective  existence.  The  situation  and  curva- 
ture of  these  rays  and  the  apparently  vacant  spaces  where  such 
rays  seem  to  be  wanting  (the  so  called  "rifts-")  can  be  accu- 


PLATE  VIII. 


DIAGRAM  ILLUSTRATING  VARIATION  IN  THE  CURVATURE  AND  POSITION 
OF  A  SINGLE  STREAMER  IN  PROJECTION,  BY  J.  M.  SCHAEBERLE. 


By  J.  M.  Schaeberle.  57 

rately  observed,  and  the  present  theory  enables  one  to  account 
for  such  rays  and  rifts,  and  to  give  the  inclinations  and  general 
directions  of  their  curvatures. 

We  will  now  proceed  to  investigate  the  curvatures  and  situa- 
tions of  the  polar  rays,  first  deducing  the  expressions  which 
give,  in  projection,  the  positions  and  curvatures  of  the  streamers. 

I  call  a  "  streamer  "  the  actual  stream  of  particles  ejected 
from  the  Sun.  I  call  a  "ray"  the  subjective  appearance  pro- 
duced by  overlapping  streamers  seen  in  projection,  and  I  write 
"ray"  in  italics. 

We  will  first  consider  the  problem  for  the  case  when  fi=Q. 
Let  t  denote  the  heliocentric  longitude  of  the  base  of  a  streamer 
in  latitude  q>,  and  let  the  longitude  of  the  Earth  be  r0,  the  plane 
of  the  Sun's  equator  being  taken  as  the  fundamental  plane.  A 
normal  in  latitude  (p  and  longitude  r  —  r0  will  in  projection  inter- 
sect the  Sun's  limb  at  a  polar  distance  p  given  by  the  equation: 

-)  (12) 


The  position  angle  p'  of  the  inclined  stream  for  moderate  polar 
distances  can  then  be  found  from  the  approximate  expression: 

cos    T—T° 


The  inclination  (  J")  of  the  stream  to  a  normal  through  its 
base  will  in  projection  be  given  by  the  approximate  expression: 

__I  COS(T—TO) 


Finally,  the  inclination  I'  to  a  normal  passing  through  the 
point  at  which  the  inclination  is  required,  will  be  approxi- 
mately : 

r=r-(p-p')  (15) 

Now,  owing  to  the  inclinations  of  the  streamers,  it  is  at  once 
evident  that  even  when  they  are  uniformly  distributed  in  longi- 
tude, they  can  never  be  symmetrically  arranged  around  a  radius- 
vector  of  the  Earth.  In  projection,  however,  an  approach  to 
a  symmetrical  form  results  from  a  peculiar  but  well  known 
optical  phenomenon. 

The  streamers  which  have  the  least  inclination  to  the  line  of 
sight  will  evidently  appear  to  be  most  widely  separated;  that 
is,  they  will  always  be  at  the  areas  of  minimum  density.  For 
the  nearer  hemisphere  the  minimum  density  in  projection  will 


58        A  Mechanical  Theory  of  the  Solar  Corona, 

evidently  always  be  just  a  little  to  the  west  of  the  Sun's  pole, 
while  for  the  farther  hemisphere  it  will  be  to  the  east  of  the 
Sun's  pole. 

Again,  as  the  streamers  are  slightly  curved,  those  having  the 
least  inclination  to  the  line  of  sight  will  in  projection  appar- 
ently have  the  greatest  inclination  with  reference  to  normals. 
Hence,  when  the  Earth  is  near  either  node,  an  approximately 
uniform  distribution  in  longitude  of  streamers  from  a  given 
latitude  cp  will  result  in  the  following  arrangement  in  ortho- 
graphic projection: 

As  streamers  issuing  from  the  nearer  hemisphere  have  an 
eastward  inclination  with  reference  to  normals,  the  two  areas 
of  minimum  density  will  be  a  little  to  the  west  of  the  Sun's 
poles;  while  for  the  farther  hemisphere  as  the  streamers  have 
a  westward  inclination  with  reference  to  normals,  the  corre- 
sponding areas  of  minimum  density  will  be  a  little  to  the  east 
of  the  Sun's  poles. 

The  inclination  to  the  normal  is  greatest  near  the  points  of 
minimum  density,  and  this  inclination  gradually  grows  less 
and  the  density  greater  as  the  angular  distance  from  these 
points  increases,  until  the  polar  distance  90° — cp  is  reached, 
where  the  inclination  to  the  normal  is  practically  zero,  and  the 
density  at  a  maximum.  ( See  illustrations  of  model,  Plate  VIII. ) 

The  apparent  intersections  of  these  streamers  produce  false 
streamers,  which  I  have  called  rays,  to  distinguish  them  from 
the  streamers  proper. 

The  form  of  these  rays  for  a  theoretical  corona  can  be  deter- 
mined after  the  method  which  will  now  be  considered. 

THEORY  OF  THE  INCLINED  RAYS. 

From  a  series  of  experiments  I  have  derived  the  expressions 
given  below,  which  govern  the  formation  of  certain  luminous 
lines  (which  for  want  of  a  specific  name  I  shall  simply  call 
rays)  produced,  as  is  well  known,  by  the  overlapping  of  two 
or  more  sets  of  alternate  bright  and  dark  lines. 

If  a  set  of  parallel  luminous  lines,  separated  by  the  small 
angular  distance  D,  is  crossed  at  the  small  angle  J  by  a  second  set 
of  parallel  lines  separated  by  the  slightly  less  angular  distance  D', 
then  when  either  set  is  viewed  through  the  other,  a  new  and  heavier 
set  of  luminous  lines  (rays)  will  be  formed,  which  make  the  angle 


By  J.  M.  Schaeberle.  59 

K  with  the  wider  set  of  lines,  and  the  angle  K  —  /  with  the  set  of 
closer  lines. 

I  have  deduced  the  following  rigorous  expression  for  the 
value  of  K: 

:  ^:   ;   tan  K=D=W^J^  J     ,     <16) 

The  perpendicular  distance  D1  between  two  adjacent  lines 
(rays)  of  the  new  set  is  given  by  the  rigorous  expression: 

D1=D(cot  /—cot  J5T)sin  K  (17) 

Equation  (16)  shows  that  K  is  always  greater  than  J,  and 
reaches  a  maximum  when  D  —  D'sec  J=0;  for  this  condition 
K=90°  and  D1=Z)  cot  /. 

As  the  angle  /  increases,  the  number  of  intersections  to  a 
given  surface  increases.  Now  as  these  intersections  cause  the 
phenomenon  of  the  inclined  rays  (a  ray  passes  through  those 
intersections  which  are  nearest  together),  it  is  evident  that  the 
rays  will  be  least  conspicuous  when  the  number  is  greatest, 
since  the  contrast  between  different  parts  of  a  surface  covered 
by  such  rays  diminishes  as  the  intervals  grow  smaller. 

If  one  of  the  two  sets  of  lines  is  doubled  by  interpolating  a 
new  line  midway  between  each  of  two  adjacent  lines,  a  new  ray 
will  be  formed  midway  between  each  of  the  original  rays. 

Similarly,  if  both  sets  of  lines  be  supposed  to  change  in  the 
same  way,  precisely  the  same  effect  will  be  produced,  the  num- 
ber of  rays  being  quadrupled. 

If  this  process  of  bisection  is  continued  indefinitely,  a  limit 
is  soon  reached  at  which  the  lines  and  rays  form  a  practically 
continuous  surface.  The  inclination  of  these  rays  always  remains 
parallel  to  the  original  direction  corresponding  to  the  particu- 
lar condition  D  —  D'=x\  the  K  for  this  particular  series  of  rays 
can  be  distinguished  from  other  series  of  less  conspicuous  rays, 
made  by  the  same  set  of  lines,  by  writing: 


)sec.  j 

The  values  of  K  for  each  of  the  other  sets  of  inconspicuous 
rays  can  be  found  by  substituting  in  (17'),  successively,  the 

D'  D'    T)f  Df 

values  2~,  -j-,  -^-  ______  ^ir,  in  place  of  D'. 

The   most   favorable    case    for   conspicuous   rays   evidently 


60        A  Mechanical  Theory  of  the  Solar  Corona, 

results  when  /  is  small,  and  D  —  D'=x  (x  being  a  small  quan- 
tity), since  for  these  conditions  any  two  intersecting  lines 
have  many  points  in  common,  supposing  the  lines  to  have 
sensible  breadths,  and  only  one  value  of  K  is  possible,  so  that 
all  the  rays  are  inclined  in  the  same  direction,  thus  at  once 
rendering  them  unmistakable. 

Equation  (17)  shows  that  so  long  as  J  is  very  small,  the 
number  of  rays  increases  very  rapidly  as  J  increases.  For 
large  values  of  J",  therefore,  no  conspicuous  rays  will  be  shown. 

As  the  angle  /—  27'  will  always  be  small  so  far  as  the  pres- 
ent investigation  is  concerned,  we  can,  without  appreciable 
error,  write,  in  place  of  equation  (16),  the  expression: 

tanJfiT=7tan  /  (18) 


I  tried  to  deduce  a  rigorous  expression  for  the  equation  of 
the  curve  formed  by  the  projection  of  the  nearer  set  of  stream- 
ers upon  the  farther  set,  but  found  the  conditions  too  compli- 
cated, since  there  are  two  sets  of  curved  diverging  lines,  neither 
set  having  a  common  point  of  intersection,  and  the  two  sets 
having  different  envelopes,  while  the  angle  of  divergence  itself 
is  a  variable  quantity. 

We  can,  however,  apply  the  above  formula  for  finding  K,  if 
we  consider  only  very  short  portions  of  the  curve,  since  for 
very  short  distances  the  deviation  from  parallelism  of  two 
adjacent  streamers  will  be  small,  and  consequently  the  error  in 
K  will,  as  a  rule,  be  small  also. 

Now  for  a  series  of  normals,  radiating  at  regular  intervals 
from  a  small  circle  whose  latitude  is  (p,  the  angle  between  the 
normals  in  the  nearer  and  farther  hemispheres  for  the  same 
position-angle  p  is  always  zero  in  projection;  hence  K  is  always 
zero,  whatever  the  relative  density  of  the  normals  in  the  two 
hemispheres  may  be.  The  projected  intervals  will  not  vary  as  a 
function  of  p  alone,  since  for  normals  in  latitude  cp,  the  density 
will  be  at  a  maximum  when  £>=90°  —  cp]  hence  it  follows  that 
the  intervals  vary  as  some  function  of  ap,  a  being  defined  by: 


Now,  in  the  case  of  an  actual  streamer,  when  the  base  is  in 
longitude  T  —  r0,  the  longitude  indicated  by  the-  direction  of  the 


By  J.  M.  Schaeberle.  61 

stream  at  a  distance  p  from  the  base  will  be  (T  —  TO  —  /');  hence, 
when  the  direction  of  the  streams,  at  a  distance  p,  corresponds  to 
T  —  r0—  0  and  r  —  TQ=180°,  the  bases  of  these  streams  will  be 
in  longitudes  -f/'  and  180°-^!',  respectively.  Now,  in  projection, 
the  position-angles,  p^  and  p2  corresponding  to  these  longitudes, 
are  given  by  the  approximate  expressions: 

u-n     T 
PI=  -~s~^-  -*> 

.....  •''  >-"•'  ••       +£t£J_+/  (20) 

^2~~  ~ 


In  which  1=6  —  (GO  —  &>Q),p  being  measured  from  the  north 
pole  towards  the  east,  through  360°. 

P-L  and  p2  will  be  called  the  secondary  coronal  poles  of  the 
nearer  and  farther  hemispheres,  respectively,  for  the  latitude  cp. 

The  location  of  the  secondary  poles  can  perhaps  be  better 
understood  from  what  follows. 

At  the  north  pole,  for  example,  streamers  from  the  nearer 
hemisphere,  which  are  projected  on  the  west  side  of  the  second- 
ary pole,  appear  to  radiate  from  points  which  are  below  the 
Sun's  center.  As  the  position  angle  increases,  the  center  of 
divergence  appears  to  approach  the  Sun's  center,  and  then  to 
rise  above  it,  so  that  streamers  on  the  east  side  appear  in  pro- 
jection to  radiate  from  points  above  the  Sun's  center. 

Consequently,  at  the  same  true  polar  distances,  the  density 
on  the  east  side  of  the  Sun  will  be  greater  than  it  is  on  the 
west  side.  For  the  streamers  of  the  farther  hemisphere  pro- 
jected at  the  same  pole,  the  arrangement  is  evidently  exactly 
the  reverse. 

A  streamer  is  at  a  secondary  pole  when  its  direction  in  projec- 
tion is  parallel  to  the  Sun's  axis. 

Equation  (16)  can  -be  written: 

tan  K=  -  L_tan/  (21) 


From  which  it  appears  that  K  is  only  dependent  on  the  'ratio 
of  D'  to  Z),  and  entirely  independent  of  their  absolute  values. 

Let  us  consider  /  to  be  positive  when  the  inclination  of  the 
denser  set  of  projected  streamers  to  the  less  dense  set  is  in  the 


62        A  Mechanical  Theory  of  the  Solar  Corona, 

direction  N.E.S.W.,  and  negative,  when  the  inclination  is  in 
the  opposite  direction;  then,  in  conformity  with  the  law  stated 
on  page  58,  the  factor: 

D 
D—D' 

will  be  positive  in  the  first  and  second  quadrants  (but  inde- 
terminate between  the  limits  ^=90° — cp  and  90°+ q>),  and 
negative  in  the  third  and  fourth  quadrants  (but  indeterminate 
between  the  limits  p=27Q°—<p  and  270°+^);  hence,  ac- 
cording to  the  above  equation,  K  will  always  have  the  same 
sign  as  J,  or,  in  other  words,  the  rays  in  latitudes  greater  than 
q>  will  always  be  inclined  in  a  direction  away  from  the  nearer 
pole.  The  angle  which  the  ray  makes  with  a  normal  will  be 
K — /•«/,  but  as  /  is,  as  a  rule,  smaller  than  the  error  of  the 
measured  inclinations,  and  /  always  less  than  0.5,  the  term  // 
can  be  neglected.  K  can  therefore  be  considered  to  be  the 
inclination  of  the  ray  to  a  normal,  and  if  the  quadrant  is 
mentioned  no  attention  need  be  paid  to  the  sign  of  K,  as  the 
inclination  is  in  the  direction  away  from  the  nearer  pole. 

For  finite  values  the  condition  D=D'  will  only  be  fulfilled  at 
the  poles  where  the  density  is  near  a  minimum;  the  very  short 
concentric  arcs  formed  by  the  few  intersections  of  nearly  normal 
streamers  inclined  to  each  other  at  the  small  angle  J,  will  there- 
fore not  be  visible  as  a  rule.  The  nearly  normal  rays  at  the 
poles,  therefore,  nearly  coincide  with  the  streamers.  This  par- 
ticular phase  of  the  phenomenon  is  beautifully  illustrated  by 
means  of  the  models  given  in  Plate  VII.,  described  further  on. 
Figure  I.  illustrates  one  of  the  cases  which  correspond  to  the 
the  value  /?=0°,  so  that  in  orthographic  projection  D=Df  at 
the  poles;  for  this  exceptional  position  the  slightest  variations 
of  the  angle  J,  produced  either  by  elevating  one  set  of  lines  with 
respect  to  the  other,  or  by  a  rotary  motion  of  the  plates,  causes 
the  ray  to  swing  very  rapidly  through  a  large  angle,  producing 
forms  like  Figures  II.,  III.,  IV.,  XV.,  all  corresponding  to  small 
values  of/.  (Figures  X.  and  XI.  represent  conditions  when  J 
is  comparatively  large  and  D=D'.)  Except  for  critical  cases, 
a  given  value  of  IT  does  not  change  to  any  great  extent  for  small 
relative  variations  of  Z),  Z)',  J,  as  can  be  seen  from  an  inspec- 
tion of  the  figures.  At  the  same  position-angle  p  the  value  of 
K  will  vary  but  slightly  when  p  is  comparatively  large,  and 


By  J.  M.  Schaeberle.  63 

although  the  apparent  changes  are  very  rapid  for  a  given  ray, 
yet  as  each  one  assumes  a  new  position  another  ray  is  formed 
which  nearly  occupies  the  successive  positions  of  the  preceding 
ray,  so  that  at  any  given  instant  the  apparent  change  in  the 
whole  system  of  rays  will  only  result  in  a  lateral  displacement 
of  the  axis  of  symmetry,  and  for  the  critical  cases  the  concen- 
tric rays  formed  are  usually  not  of  sufficient  magnitude  to  be 
seen,  as  has  been  explained  above.  When  both  sets  of  stream- 
ers are  visible,  the  pyramidal  form  of  the  denser  portions  of  the 
rays  projected  at  the  poles  can  be  regarded  as  resulting  directly 
from  the  overlapping  of  streamers  inclined  to  each  other. 

Now  the  streamers  at  the  nearer  secondary  pole  are  projected 
against  streamers  of  the  farther  hemisphere,  which  are  at  an 
angular  distance  of  2/(— /)  from  the  farther  secondary  pole; 
for  the  polar  distance  p  the  ratio  of  the  intervals  D  and  Dr  is 
therefore  a  function  of  ap  and  /'.  This  function  must  be  so  deter- 
mined that  the  density  is  least,  but  not  zero,  when  p=0  ±  /', 
and  a  maximum  finite  density  when  p=9(j0 — g>,  or  op=90°. 

Let  d  and  $'  denote  the  densities  of  the  two  sets  of  streamers 
for  a  given  polar  distance  p.  We  then  have  as  a  rough  approx- 
imation for  values  of  p  greater  than  / : 

d=d  sin  (ap+IJ 
d'=d  sin  (ap—Ij 
The  value  of  d  being  determined  by  the  condition: 

(23) 


In  which  <?0  is  the  density  at  the  true  pole. 

In  place  of  the  density  #,  we  can,  for  moderate  polar  dis- 
tances, substitute  the  reciprocal  of  the  corresponding  interval 
Z),  and  write: 

|     *=!       *=£  (24) 

Hence: 


D        cT~sin 

Substituting  this  value  of  the  ratio  of  the  intervals  in  equa- 
tion (21),  and  reducing,  we  obtain,  finally: 

tan  K  =    sin<ffl?-J)  r  tan  2T  (26) 

2cos  (ap)  sin  / 


64        A  Mechanical  Theory  of  the  Solar  Corona, 

21'  being  substituted  in  place  of  /.  As  /'  is  small  we  can 
write  tan  2/'=2  tan/';  hence, 

tan  K=   8i"   (af~Jl)r  tan  T  (27 ) 

cos  (ap)  sin  Y! 

The  ratio  of  tan  /'  to  sin  /x  will  be  practically  constant  for 
moderate  values  of  p.  When  ajp— 90°,  equation  (27)  becomes 
indeterminate.  If  the  streamers  were  of  infinitesimal  breadth 
in  latitude,  they  would  coincide  with  the  rays  when  p=90° — q>. 
In  reality,  however,  the  extension  in  latitude  may  be  consider- 
able, and  the  effect  of  this  extension  is  to  make  a  practically 
continuous  surface  of  rays  before  the  polar  distance  is  as  great 
as  90° — cp.  Hence,  polar  rays  at  considerable  polar  distances 
will  usually  be  lost  in  the  general  illumination. 

From  the  preceding  discussion  it  follows  that  for  the  case  of 
/3=Q°  the  axis  of  the  typical  corona  will,  in  orthographic  pro- 
jection, coincide  with  the  Sun's  axis. 

CHANGES  IN  THE  FORM  OF  THE  TYPICAL  CORONA  RESULTING 
FROM  VARIATIONS  IN  THE  HELIOCENTRIC  LATITUDE  OF  THE 
EARTH. 

• 
When  the  Earth  is  above  (/?+)  or  below  (ft — )  the  plane  of 

the  Sun's  equator,  the  quantities  Z>,  D\  and  /  undergo  certain 
changes  for  the  same  value  of  p  in  projection. 

When  the  Earth  is  below  the  plane  of  the  equator,  the  nearer 
streamers  of  tl^e  northern  hemisphere  will  appear  more  dense, 
with  a  slightly  less  inclination  to  the  normal  than  is  the  case 
when  /?=0,  while  the  density  of  the  streamers  from  the  farther 
hemisphere  will  be  diminished;  but  the  increase  in  the  west- 
ward inclination  to  the  normal  will  be  greater  than  the  dimi- 
nution of  the  eastward  inclination  in  the  nearer  hemisphere. 
j  has  therefore  increased,  but  this  increase  is,  in  part,  at  least, 

counteracted  by  the  decrease  in  the  value  of  the  factor  —=^ — =r,. 

With  reference  to  the  streamers,  therefore,  K  does  not  neces- 
sarily change  to  any  great  extent.  But  as  the  nearer  streamers 
have  a  less  eastward  inclination,  while  the  farther  ones  have  a 
greater  westward  inclination,  the  whole  system  of  rays  formed 
will,  according  to  the  fundamental  principle  laid  down  in  the  law 
given  on  page  58,  have  a  greater  eastward  inclination.  The 


By  J.  M.  Schaeberle.  65 

effect  of  this  common  change  in  the  inclination  of  the  rays  is  to 
cause  an  apparent  shifting  of  the  coronal  pole  towards  the  WEST. 

For  the  same  reason  the  south  coronal  pole  will  be  shifted 
towards  the  EAST. 

When  the  Earth  is  above  the  plane  of  the  equator,  the  north 
pole  of  the  corona  will  be  on  the  east  side  of  the  projected  posi- 
tion of  the  Sun's  pole,  and  the  south  coronal  pole  will  lie  on 
the  west  side. 

As  the  projections  seen  from  the  Earth  are  not  strictly  ortho- 
graphic, the  parallactic  effect  has  a  constant  tendency  to  throw 
both  coronal  poles  slightly  towards  the  east  of  the  position  they 
would  occupy  if  viewed  from  an  infinite  distance. 

Changes  in  the  form  of  the  typical  outer  corona,  due  to  varia- 
tions in  ft,  for  streamers  of  a  given  magnitude  and  distribution, 
can  be  readily  understood,  with  the  aid  of  the  prints  and  dia- 
grams given  in  Plates  VI.  and  VIII.,  in  connection  with  Tables 
IV.  and  V.,  and  also  from  what  follows  further  on. 

A  want  of  uniformity  in  the  distribution  of  the  streamers  in 
longitudes  r — rQ  =  ±0,  or  180°,  may  result  in  the  partial  or 
total  destruction  of  the  symmetrical  inclined  polar  rays,  and  in 
other  longitudes  the  same  irregularities  will  cause  a  deforma- 
tion of  the  general  typical  features  of  the  corona.  An  unsym- 
metrical  corona  is,  therefore,  in  no  way  to  be  regarded  as 
contrary  to  the  theory. 

If,  for  any  cause,  there  is  real  or  apparent  periodic  variation 
in  the  mean  latitude  of  the  streamers,  the  ratio  of  the  polar  to 
the  equatorial  extension  will,  of  course,  be  subject  to  a  similar 
variation.  (See  postscript.) 

From  Table  IV.,  we  see  that  for  two  streamers  in  latitude  15° 
and  30°,  respectively,  just  visible  at  the  poles  in  projection,  the 
one  in  latitude  30°  will  have  only  about  one  third  of  the 
equatorial  extension  that  is  shown  by  streamers  in  15°  latitude. 
If,  therefore,  the  mean  latitude  of  greatest  solar  activity  is 
apparently  shifted  towards  the  higher  regions  of  the  Sun-spot 
zones,  the  coronal  outlines  may  become  practically  circular. 
The  criterion  for  determining  from  the  observed  outlines 
whether  ft  is  large  or  small  will  no  longer  be  satisfactory,  since 
the  ratio  of  the  polar  to  the  equatorial  extension  now  under- 
goes but  a  slight  change  for  all  possible  values  of  ft.  However, 
when  the  polar  rays,  or  the  wing  boundaries  adjacent  to  the  poles, 
5 


66        A  Mechanical  Theory  of  the  Solar  Corona, 

are  present,  the  position  of  the  axis  of  the  inner  corona  will,  as 
a  rule,  at  once  tell  whether  the  observer  was  above,  below,  or 
in  the  plane  of  the  Sun's  equator.  The  inclinations  of  the 
boundaries  of  the  wings,  at  the  Sun's  outline,  can  be  used  to 
indicate,  approximately,  the  position  of  the  pole  of  the  inner 
corona  when  the  rays  are  wanting. 

Now,  when  the  Earth  is  at  considerable  distances  above  or 
below  the  plane  of  the  Sun's  equator,  and  the  equatorial  stream- 
ers are  visible  for  only  a  moderate  distance,  the  more  depressed 
set  may  show  so  faintly  that  they  apparently  fall  short  of  reach- 
ing the  pole  in  projection.  For  this  case,  equation  (16)  shows 
that  K=Q,  since  2/'  is  then  zero;  so  that  if  all  the  streamers 
were  confined  to  a  single  circle  of  latitude  and  only  one  set  vis- 
ible at  the  pole,  the  true  projections  of  the  streamers  would  be 
seen,  and  the  direction  of  curvature  would  always  be  governed 
by  rigorous  conditions.  (See  Plate  VIII.) 

For  this  case,  when  the  symmetrical  inclined  rays  are  present, 
the  phenomenon  admits  of  the  same  simple  explanation,  which 
accounts  for  the  polar  rays  when  /3  is  nearly  zero,  since  stream- 
ers on  opposite  sides  of  the  Sun,  whose  latitudes  differ  by  2/?, 
will,  in  projection  at  the  poles,  produce  a  similar  arrangement 
of  the  rays;  but  these  rays  will  not  necessarily  extend  to  the 
outer  limit  of  the  coronal  structure  at  the  poles,  and  for  this 
reason  they  may  not  be  conspicuous  when  ft  is  large. 

When,  however,  the  polar  rays  are  very  conspicuous  and 
uniform  for  large  values  of  /?,  and  a  small  equatorial  extension, 
the  phenomenon  is  still  to  be  accounted  for  in  the  same  general 
way,  which  we  will  now  consider. 

As  the  curvature  and  deviation  from  the  normal  depend  in 
projection  upon  the  latitude  q>,  streamers  in  different  latitudes 
with  nearly  the  same  longitude  will,  in  projection,  apparently 
intersect  each  other,  and  consequently  curved  rays  or  outlines 
will  be  formed,  and  these  may  be  wholly  produced  in  either  the 
nearer  or  farther  set  of  streamers.  For  the  same  position-angle 
p,  streamers  in  latitude  q>'  will  not  appear  to  radiate  from  the 
same  points  that  those  in  latitude  (p  do.  If  the  secondary  poles 
for  latitude  cp'  are  given  by  the  expressions: 

p ! '  =  —  II '  nearer  hemisphere,  /  9  ft  v 

p2'  =  +  //  farther  hemisphere, 

Then  for  -f-  <p'  greater  than  -f  9  we  would  always  have  //  less 
than  II.  This  results  directly  from  the  fact  that  the  change  in 


By  y.  M.  Sckaeberle.  67 

the  directions  of  the  streams  varies  nearly  with  p2,  and  in  pro- 
jection at  the  poles  the  ratio  of  p  to  pf  is  nearly  the  same  as  the 
ratio  of  cosec  (p  to  cosec  cp' '.  The  streamers  in  latitude  cp  will 
therefore  be  more  inclined  to  the  normal  than  those  in  latitude 
cp'.  In  projection,  therefore,  streamers  on  the  east  side  of  the 
secondary  pole  in  latitude  cp  will  appear  to  radiate  from  points 
which  are  nearer  than  the  corresponding  points  for  latitude  cpf, 
while  on  the  west  side  of  the  Sun  the  points  on  the  osculating 
curves  are  at  greater  distances  for  latitude  cp  than  they  are  for 
the  latitude  cp'.  The  resulting  apparent  variation  in  density  will 
therefore  produce  the  same  phenomenon  which  results  from  the  pro- 
jection of  the  streamers  of  the  nearer  hemisphere  upon  those  of  the 
farther.  Inclined  polar  rays  may  therefore  be  formed  by  the  over- 
lapping of  streamers  having  nearly  the  same  longitude  but  differ- 
ent latitudes.  For  this  case  the  II  of  equation  (24)  would  be 
the  angular  distance  between  the  secondary  poles  for  latitude 
cp  and  cp',  while  /'  would  correspond  to  the  difference  of  the  pro- 
jected inclinations  at  the  pole  for  the  given  latitudes. 

If  we  assume  the  ratio  of  the  latter  to  the  former  to  be  c, 
and  neglect  the  small  angle  (II — .//),  equation  (27)  reduces  to: 

tan  K=c  tan  (ap')  (29) 

In  which  p'  is  nqw  the  distance  from  the  mean  secondary  pole. 
This  system  of  rays  will  be  more  probable  for  large  values  of 
ft,  and  will  not  be  symmetrical  with  reference  to  the  poles  of 
the  Sun.  The  inclinations  will  vary  with  the  value  of  c;  these 
variations  will,  however,  as  a  rule,  be  small,  since  the  values 
of  ft,  cp,  and  cp'  are  subject  to  comparatively  small  variations. 

When  ft  is  zero,  the  streams  of  the  nearer  hemisphere  pro- 
jected against  those  of  the  farther  hemisphere  will  produce  a 
corona  whose  axis  will  be  practically  coincident  or  parallel  with 
the  Sun's  axis.  The  density  (in  projection)  at  the  poles  may  at 
times  be  so  great  that  only  the  wings  are  seen;  the  boundary  of 
these  wings,  even  at  the  poles,  will  then  extend  to  a  limit  at 
which  the  polar  rays  begin. 

Equation  (21)  shows  that  the  inclination  of  the  rays  is  inde- 
pendent of  the  magnitude  of  the  intervals,  so  that  even  when 
the  density  is  very  great  or  very  small,  the  inclination  K  of  the 
polar  rays,  when  these  are  present,  will,  for  a  given  value  of  /?, 
always  be  practically  the  same  for  a  uniform  distribution  of  the 
streamers. 


68        A  Mechanical  Theory  of  the  Solar  Corona, 

The  four  great  curves  which  bound  the  outer  portions  of  the 
wing-like  coronal  outlines,  which  form  a  prominent  feature  of  so 
many  eclipses,  are  the  envelopes  of  the  outer  portions  of  the 
streamers,  the  density  at  points  on  the  envelopes  being  such 
that  the  intervals  are  just  filled  out.  The  positions  of  these 
envelopes  are  largely  determined  by  the  projection  of  the  more 
depressed  set  of  streamers  against  the  more  elevated  set,  or 
vice  versa.  (See  Plate  VI.) 

To  obtain  an  approximate  analytical  expression  for  these 
envelopes,  let  y\  be  the  distance  from  the  Sun's  center  to  the 
point  on  the  Sun's  axis,  where  one  set  of  streamers  in  latitude 
<p,  produced  backward,  would,  in  projection,  just  form  a  con- 
tinuous surface,  and  let  P'  be  the  polar  distance  of  the  point 
where  the  boundary  of  this  continuous  surface  cuts  the  limb  of 
the  Sun  in  projection.  Then  the  distance  yf,  at  which  the  inter- 
vals between  adjacent  streamers  will  just  be  filled  out  for  differ- 
ent values  of  p,  will  be  approximately  given  by  the  expression: 

yf=yi  sec  (ap)  (30) 

In  which  y\  *s  a  function  of  the  actual  density,  and  equal  to 
the  distance  from  the  Sun's  center  to  the  point  where  the 
envelope  proper,  or  the  envelope  produced,  cuts  the  Sun's  axis. 

For  values  of  ;//,  less  than  the  Sun's  radius,  the  approxi- 
mate expression  (31)  will  answer: 

„,,_         1 

sec  (al*)  (31) 

For  the  envelope  of  the  other  set  of  streamers,  projected  at 
the  same  pole,  we  have: 

y=yf  sec  (ap)  (32) 

f=^FT  (88) 

Similarly,  streamers  in  latitude  <pf,  <p",  etc.,  will  have  envel- 
opes of  the  same  general  character.  The  overlapping  of  all 
these  envelopes  finally  produces  the  outlines  of  the  four  great 
wings. 

The  principal  boundary  curve  or  curves  wTill  be  approx- 
imately represented  by  the  equation: 

y=yisec(ap)  (34) 

The  value  of  yl  being  found  from  data  taken  directly  from 
the  photographs. 


By  J.  M.  Schaeberle.  69 


Equation  (34)  is  the  locus  of  a  curve  of  indefinite  extent, 
which  leaves  the  Sun's  surface  at  the  polar  distance  P,  or  cuts  the 
Sun's  axis  at  a  distance  y\  from  the  Sun's  center,  the  inclination 
to  the  normal  varying  from  90°  for  p=0  to  0°  for  p=90° — q>. 
The  curve  has  for  its  asymptote  a  produced  diameter  of  the 
Sun  in  a  position-angle  nearly  equal  to  90° — cp  ,  in  which  cpm 
is  the  mean  latitude  of  the  streamers. 

If  the  distribution  of  the  streamers  in  longitude  is  not  uni- 
form, equation  (34)  will  not  necessarily  represent  the  observed 
form  for  small  values  of  p,  and  if  the  terrestrial  atmospheric 
conditions  are  unfavorable  for  showing  the  outer  corona,  the 
same  equation  will  apparently  fail  when  p  is  large. 

The  inner  boundaries  of  these  wings  will  be  determined  by 
similar  conditions.  As  the  forces  at  the  equator  are  presum- 
ably less  active  than  those  having  a  small  latitude,  the  envel- 
ope of  these  portions  of  the  projected  streams  will  in  general  be 
concave  near  the  Sun's  disk.  The  closing  of  the  wings  (or 
fish  tails  as  they  are  sometimes  called)  and  the  decrease  in 
density  of  the  exterior  boundaries,  result  directly  from  a  grad- 
ual increase  in  the  value  of  ft. 

The  trumpet-shaped  outline  of  the  more  distant  portions  of 
the  wings  which  were  first  photographed  in  January,  1889,  is 
theoretically  just^  what  is  called  for.  Since  the  brightness  of 
the  streamers  decreases  with  increasing  distances  from  the 
Sun's  surface,  the  illumination  can,  by  contrast,  only  be  of 
indefinite  extent  in  those  directions  where  many  of  these  stream- 
ers overlap  each  other,  that  is,  in  position-angles  corresponding 
to  ±(90°— <p)  and  ±(270°—^).  The  equation  of  the  outer 
boundary  curve  is  nearly  of  the  form  expressed  by  formula 
(34). 

The  figures  given  in  Plate  VI.  would  be  still  more  strikingly 
similar  to  coronal  outlines  were  it  practicable  to  represent  the 
decrease  in  the  brightness  of  the  streamers  (represented  by  the 
needles  in  the  model)  with  increasing  distances  from  the  center. 

POLAR  GAPS  OR  EIFTS. 

There  are  several  different  causes  which  unite  to  produce  an 
apparent  extinction  of  the  polar  rays  for  increasing  polar  dis- 
tances. The  first  of  these  is  made  evident  from  the  following 
considerations:  Viewed  from  a  given  point,  a  series  of  equally 


70        A  Mechanical  Theory  of  the  Solar  Corona, 

bright  radial  lines  (and  practically  equidistant  from  the  ob- 
server) of  indefinite  extent  will  not  appear  equally  bright  to  the 
eye.  The  lines  which  are  less  inclined  to  the  visual  rays  will 
always  be  brighter  than  the  more  inclined  ones,  since  in  a  given 
direction  the  density  of  the  luminous  particles  which  make  up 
the  line  increases  for  decreasing  inclinations.  Hence,  at  a  given 
actual  distance  from  the  Sun,  a  streamer  will  appear  brightest 
when  it  is  projected  at  the  poles. 

A  second  reason  why  the  rays  at  the  pole  are  the  brightest  is 
the  following:  Beams  from  two  sources  of  light  of  the  same  abso- 
lute quantity,  but  of  different  angular  magnitude,  will  be  affected 
differently  in  passing  through  an  absorbing  medium  like  our 
atmosphere.  If  in  one  case  the  light  is  concentrated  in  a  series 
of  points  or  lines  in  a  given  surface,  and  in  the  other  case  the 
same  amount  of  light  is  distributed  over  the  whole  of  the  same 
surface,  the  absorbing  effect  of  our  atmosphere,  through  which 
the  two  sets  of  luminous  beams  pass,  will  be  more  marked  in  the 
latter  case  than  it  will  in  the  former.  Referring  now  to  the 
illustrations  given  in  Plate  VII.,  it  will  be  noticed  that  the 
number  of  rays  increases  with  the  inclination,  while  the  mag- 
nitude of  these  same  rays  decreases  with  the  inclination.  (In 
order  that  the  outer  extremity  of  an  inclined  ray  shall  be  at  as 
great  a  distance  from  the  Sun's  limb  as  a  ray  at  the  pole,  the 
ratio  of  the  length  of  the  former  to  the  length  of  the  latter 
must  be  nearly  as  sec  K  to  unity;  or,  for  the  same  length  of 
inclined  and  polar  rays,  the  corresponding  ratio  of  distances 
from  the  Sun's  limb  would  be  nearly  as  cos  K  to  unity. )  The 
absorbing  effect  of  our  atmosphere  wrill  therefore  always  have 
the  tendency  to  cause  a  greater  weakening  of  the  more  inclined 
rays  up  to  the  position  where  the  increase  in  density  suddenly 
rises  in  projection  (in  the  model  this  absorptive  effect  is  of 
course  not  included,  hence  the  gaps  are  not  strongly  shown), 
the  effect  of  which  is  to  cause  a  great  contrast  between  the 
comparatively  bright  boundaries  of  the  wings  and  the  more 
conspicuous  polar  rays.  An  inspection  of  the  best  photographs, 
however,  will  show  that  these  spaces,  apparently  devoid  of 
dense  coronal  matter,  are  often  really  filled  out  with  faint  rays, 
which  in  a  poor  photograph  would  not  show  at  all.  The  exist- 
ence of  rifts  in  other  positions  is  illustrated  in  the  models. 
When  the  density  of  the  streamers  is  so  small  that  no  definite 


By  J.  M.  Schaeberle.  71 


boundary  of  a  wing  is  formed,  the  rays  may  be  visible  to  a  polar 
distance  nearly  equal  to  90° — (p.  Even  if  the  streamers  are  not 
of  a  gaseous  character,  their  boundaries  will  not  be  sharply  de- 
fined, since  the  variation  in  latitude  results  in  intersections  at 
very  small  angles;  any  attempt,  therefore,  to  follow  the  course  of 
any  particular  one  of  these  streamers,  projected  as  it  is  against 
many  others,  may  be  wholly  in  vain. 

GRAPHICAL  REPRESENTATION  OF  POLAR  RAYS. 

In  the  model  (Plate  VI.)  the  diameter  of  the  needles  com- 
pared with  the  diameter  of  the  ball  is  too  great  to  admit  of  the 
use  of  a  sufficient  number  to  produce  the  phenomenon  of  inclined 
rays  satisfactorily. 

I  have,  however,  been  able  to  fulfill  the  conditions  imposed 
by  a  modification  of  the  graphical  method.  In  projection,  the 
streamers  near  the  poles  will  appear  to  be  tangent  to  a  small 
circle  concentric  with  the  Sun,  instead  of  passing  through  the 
Sun's  center.  Accordingly,  instead  of  using  slightly  inclined 
needles  radiating  from  the  surface  of  a  sphere,  I  formed  a  series 
of  alternate  bright  and  dark  lines  on  an  opaque  film  on  the 
surface  of  a  piece  of  plate  glass.  These  radial  lines  (slightly 
curved)  were  all  drawn  tangent  to  the  same  small  circle,  so  that 
for  a  given  distaiice  from  the  center  of  this  circle  the  inclination 
to  a  normal  was  approximately  the  same  as  required  by  theory. 
On  this  plate  a  second  plate  copied  from  the  first  was  laid,  in 
both  the  direct  and  reversed  positions. 

Now  the  condition  which  must  be  fulfilled  is  this:  The  lines 
of  one  plate  must  all  be  inclined  in  the  same  direction  with 
reference  to  the  lines  of  the  other  plate,  and  this  arrangement 
must  still  produce  rays  which  incline  away  from  the  lines  rep- 
resenting the  secondary  poles,  if  the  theory  is  true.  While  I 
had  no  doubt,  from  theoretical  considerations,  as  to  what  the 
pictorial  result  of  the  combination  of  the  two  gratings  would 
be,  I  had  hardly  hoped  to  obtain  such  satisfactory  results  on  a 
first  trial.  In  Plate  VII.,  Figures  I.,  II.,  III.,  IV.,  VIII.,  X.,  XI., 
XV.,  a  and  c  illustrate  some  of  the  many  forms  which  can  be 
produced  by  streamers  having  nearly  the  same  longitude,  but 
different  latitudes,  the  plates  for  this  purpose  being  superposed 
without  reversing.  The  remaining  prints  V.,  VI.,  VII.,  IX., 


72        A  Mechanical  Theory  of  the  Solar  Corona, 

XL,  XII.,  XIII.,  6,  d,  and  e,  illustrate  some  of  the  forms  pro- 
duced when  the  streamers  of  the  nearer  hemisphere  are  projected 
against  those  of  the  farther  hemisphere,  the  plates  being  reversed 
for  this  purpose.  The  shifting  of  the  secondary  coronal  pole  is 
also  represented  (see  Figures  VIII.  and  IX.,  Plate  VII.) ;  one  set 
of  lines  being  slightly  raised  or  lowered  to  correspond  to  a  change 
in  the  position  of  the  Sun's  axis,  which,  in  projection,  is  sup- 
posed to  be  parallel  to  the  edge  of  the  paper. 

The  original  prints  were  made  on  platinum  paper,  the  two 
superposed  gratings  representing  the  negative.  These  prints, 
like  those  of  Plate  VI.,  were  then  fastened  to  a  large  sheet  and 
photographed  so  as  to  obtain  on  a  single  page  all  the  different 
forms  shown  in  Plate  VII. 

If  a  set  of  alternate  bright  and  dark  straight  lines  radiating 
from  the  same  point  is  placed  upon  another  set  of  lines  also 
radiating  from  a  point,  no  curves  will  be  formed  so  long  as  the 
centers  of  divergence  are  in  the  same  line  of  sight;  but  the 
instant  one  center  is  shifted  with  reference  to  the  other,  curves 
quite  similar  to  those  given  in  Plate  VII.  will  be  produced. 
If  the  plates  are  separated  from  each  other,  the  errors  in  the 
directions  and  positions  of  the  lines  will  have  a  much  less  dis- 
torting effect  upon  the  rays  than  when  the  plates  are  close 
together. 

For  the  purpose  of  making  the  prints,  however,  it  was  nec- 
essary to  place  the  plates  close  to  the  platinum  paper;  all  the 
irregularities  are  therefore  shown  in  these  prints.  It  must  be 
remembered  that  from  the  nature  of  the  model  the  outer  por- 
tions of  the  rays  shown  in  the  figures  of  Plate  VII.  are  much 
too  bright  and  prominent,  since  the  intensity  does  not  diminish 
with  the  distance  from  the  center  of  divergence,  as  it  evidently 
does  for  the  actual  corona. 

Then,  again,  in  the  model  the  contrast  between  the  bright 
and  dark  lines  is  abrupt  and  sharp,  so  that  in  the  prints,  for  a 
near  view,  these  lines  show  plainly  with  the  rays',  but  in  the 
case  of  actual  streamers  this  state  of  things  would  evidently 
not  exist.  If  the  plate  is  removed  several  feet  from  the  eye, 
only  the  rays  will  be  distinguishable  to  the  unaided  vision. 

NOTE.— If  each  eruption  is  regarded  as  resulting  in  a  large  number  of  slightly 
diverging  pencils  of  matter,  two  eruptions  on  the  central  meridian  in  slightly 
different  latitudes  would,  in  projection  at  the  poles,  also  cause  the  phenome- 
non of  inclined  rays. 


By  J.  M.  Schaeberle.  73 


If  several  plates  are  superposed,  the  contrasts  are  strength- 
ened, and  grotesque  figures,  resulting  from  irregularities  in  the 
gratings,  are  not  uncommon. 

The  boundaries  of  the  wings  in  the  hemisphere  which  con- 
tains the  visible  pole  will,  even  for  comparatively  small  values 
of  /?,  usually  appear  double  or  multiple  on  the  side  turned 
toward  the  adjacent  pole,  as  portions  of  both  sets  of  streamers 
can  be  seen  directly. 

When  fi  is  exactly  zero,  and  the  density  of  the  streamers 
uniform  and  great,  the  outer  boundary  of  the  wings,  even  at  the 
poles,  may  inclose  the  area  usually  occupied  by  the  polar  rays. 
The  density  of  the  coronal  areas  will  then  increase  toward  those 
axes  whose  latitudes  are  the  same  as  the  mean  latitudes  of  the 
streamers.  The  outlines  of  the  fainter  and  more  distant  por- 
tions, rendered  visible  by  the  overlapping  of  many  faint  streamers 
projected  along  these  axes,  will  then  be  approximately  repre- 
sented by  equation  (34).  If,  however,  for  any  cause  the  stream- 
ers from  the  low  latitudes  are  not  decidedly  more  conspicuous 
than  those  in  higher  latitudes,  or  if  there  is  a  real  or  an  apparent 
periodic  increase  in  the  latitudes  of  the  streams,  which  at  times 
transfers  the  scene  of  greatest  visible  activity  to  the  higher  limits 
of  the  spot-zones,  the  outline  of  the  bounding  curves  of  the  wings 
is  more  likely  to  form  a  closed  figure,  and  the  general  coronal 
boundary  will  be  more  nearly  circular,  since  the  contrast 
between  the  areas  of  different  brightness  for  increasing  dis- 
tances may  not  be  sufficient  to  bring  out  the  envelope  whose 
approximate  equation  has  already  been  considered. 

From  what  has  already  been  said,  it  is  evident  that  the  con- 
dition of  the  Earth's  atmosphere  at  the  place  and  time  of  obser- 
vation, determines,  in  a  very  great  degree,  the  form  of  the  visible 
boundary  of  the  outer  corona. 

Before  giving  further  results  of  the  comparison  between 
theory  and  observation,  it  is  proper  to  make  a  few  remarks 
relating  to  the  difficulty  under  which  one  labors  in  making  an 
unbiased  examination  of  published  data  which  are  believed  to 
be  representations  of  a  certain  theoretical  form. 

One  is  very  apt  to  overestimate  the  importance  of  certain 
coincidences  and  to  disregard  as  unimportant  certain  discrep- 
ancies. For  instance,  some  of  the  evidence  tending  to  prove 
that  the  streamers  issue  from  the  Sun's  equatorial  regions 


74        A  Mechanical  Theory  of  the  Solar  Corona, 

depends  to  a  certain  extent  upon  the  observed  variations  of  the 
general  outlines  of  the  outer  corona  for  different  values  of  ft. 
So  far  as  this  particular  evidence  is  concerned  the  conclusion 
reached  must  depend  largely  upon  the  data  derived  from  mere 
drawings,  as  the  number  of  reliable  photographs  secured,  for 
different  eclipses,  is  hardly  sufficient  to  decide  the  case  def- 
initely. The  interpretation  of  these  drawings  and  poorer  pho- 
tographs, by  different  unbiased  observers,  will  not  necessarily 
be  the  same. 

Certain  features  should,  however,  always  be  present  in  good 
photographs,  giving  evidence  tending  to  prove  that  the  stream- 
ers originate  in  the  spot-zones;  of  these  the  equatorial  outlines 
of  the  outer  corona  are  perhaps  the  most  important.  The  vari- 
ation in  the  position  of  the  secondary  coronal  poles,  according 
to  the  position  of  the  observer  with  reference  to  the  Sun's  equa- 
tor, also  gives  decisive  evidence  on  this  point. 

For  those  eclipses  of  which  we  have  photographs  showing 
polar  rays  suitable  for  measurement,  I  have  used  the  constants 
for  a  mean  latitude  of  15°  for  the  streamers,  and  placed  /?— 0 
for  finding  K .  As  the  exact  nature  of  the  distribution  of  the 
streamers  in  latitude  is  not  known,  any  attempt  to  take  into 
consideration  the  slight  variations  in  K,  due  to  variations  of  ft 
between  0°  and  8°,  in  order  to  obtain  a  closer  agreement  between 
theory  and  observation,  would  seem  to  be  superfluous.  For 
those  photographs  of  eclipses  in  which  the  rays  are  not  shown, 
I  have  used  the  following  method  for  obtaining  the  direction 
of-  inclination  of  the  axis  of  the  inner  corona  with  reference  to 
the  Sun's  axis.  At  the  origin  of  the  curves  bounding  the  wings 
adjacent  to  the  poles,  tangent  lines  were  drawn.  Through  the 
two  points  of  intersection,  formed  by  the  two  lines  near  each 
pole,  the  coronal  axis  is  supposed  to  pass;  when  this  line  does 
not  pass  through  the  Sun's  center,  I  have  assumed  it  to  be  par- 
allel to  the  coronal  axis,  as  the  parallactic  effect  in  a  typical 
form  is  such  that  both  poles  of  the  corona  are  shifted  towards 
the  east  of  the  points  they  would  occupy  in  orthographic  pro- 
jection. The  data  for  finding  the  position  of  the  Sun's  center 
with  reference  to  the  center  of  the  Moon  is,  also,  nearly  always 
wanting. 

As  this  shifting  of  the  secondary  poles  will  ordinarily  be 
only  a  few  degrees,  I  have  preferred  to  refer  all  the  measures 


By  J.  M.  Schaeberle. 


75 


to  the  true  solar  poles,  rather  than  to  the  coronal  poles;  this 
treatment,  when  /3  is  large,  will  of  course  make  the  differences 
between  computation  and  observation  larger  than  they  would 
be  if  the  coronal  poles  were  taken  as  the  origin. 

For  the  above  named  conditions  we  therefore  have  for  the 
neighborhood  of  the  poles  and  at  the  Sun's  limb  the  following 
numerical  values: 
tan  lf 


-=c=1.5,  a=1.2,  and 


tan  g= 


Hence, 

r__1.5  sin  (1.2ff— 2°) 
cos  (1.2  p) 

The  following  are  the  numerical  values  of  K  for  each  10°  of 
distance  from  the  adjacent  pole: 


P 

10° 

20° 

30° 

40° 

K 

15° 

31° 

46° 

58° 

With  reference  to  the  form  of  the  outer  corona,  as  shown  by 
any  particular  photograph,  a  very  great  deal  depends  upon  the 
mode  of  development  of  the  photographic  plate.  A  corona  with 
great  equatorial  extension  can  be  made  to  appear  nearly  circu- 
lar, especially  if  the  atmospheric  conditions  at  the  time  of  an 
eclipse  are  poor,  so  that  only  the  brighter  parts  are  shown.  In 
dealing  with  drawings  not  made  from  photographs,  a  rude 
approximation  to  the  true  general  outline  can,  at  best,  only  be 
obtained  by  combining  the  results  of  many  different  observers 
of  the  same  eclipse.  Such  drawings  are  of  little  or  no  value 
for  determining  the  sign  of  ft.  The  individual  results  of  pure 
drawings  are  often  so  discordant  among  themselves  that  it  is 
difficult  to  comprehend  how  they  can  possibly  be  reconciled  so 
as  to  represent  the  same  phenomenon. 

Bearing  in  mind  the  fact  that  in  the  graphical  represen- 
tation the  intensity  or  distinctness  of  each  streamer  does  not 
decrease  as  the  distance  from  the  center  increases,  the  prints 
from  the  model,  of  which  illustrations  are  given  in  Plate  VI., 
can,  in  a  general  way,  be  used  to  represent  typical  coronas. 
The  outline  of  the  outer  corona  gives  a  rough  indication  of  the 
amount  of  the  inclination  of  the  Sun's  axis;  while  the  indi- 


76        A  Mechanical  Theory  of  the  Solar  Corona, 

cated  positions  of  the  poles  of  the  inner  corona  at  once 
determine  whether  the  observer  is  above  or  below  the  plane  of 
the  equator.  It  will  be  noticed  that  even  in  this  simple  model 
the  boundaries  of  the  wings  indicate  the  positions  of  the 
coronal  poles.  The  reason  why  the  polar  rays  are  not  satis- 
factorily formed  has  already  been  stated. 

TABLE  V.    (Plate  VI.) 

i 
No.  of  Figure.  Corresponds  to  Season  of  the  Year. 


t 

End  of 

November  and  beginning  of  December. 
End  of  May  and  beginning  of  June 

J 

2,  3,  and  4  !  ---    End 

of  December  and  beginning  of  January. 
End  of  July  and  beginning  of  August, 
of  January  and  beginning  of  February, 
d  of  February  and  oeginning  of  March, 
of  August  and  beginning  of  September. 

5 

6 

End 

7 

En 

8 

End 

OBSERVATIONS  OF  SOLAR  ECLIPSES  AND  COMPARISONS  WITH 

THEORY.* 

Eclipse  of  1715,  May  2. 

The  individual  drawings  and  descriptions  are  discordant 
among  themselves. 

1776,  February  9. 

Same  remarks  as  above. 

1806,  June  16. 

The  drawing  is  described  as  being  a  mere  diagram,  showing 
the  general  effect  of  the  light  about  the  dark  Moon.  Equatorial 
streamers  evidently  not  markedly  large.  (Maximum  of  spots, 
1804;  minimum,  1811.) 

1842,  July  8. 

Imperfect  records.  The  observers  supposed  the  equatorial 
extension  to  be  the  zodiacal  light.  Equatorial  extension  great. 
(Maximum  of  spots,  1837;  minimum,  1843.) 

*  All  the  references  are  to  A.  C.  RANYARD'S  work  "  Observations  made  during 
Solar  Eclipses,"  Mem.  R.  A.  S.,  Vol.  XLL,  unless  otherwise  stated.  To  make 
possible  a  comparison  between  the  variations  in  the  general  details  of  the 
corona,  as  influenced  by  the  phenomena  of  outgoing  streamers  retarded  by 
incoming  ones  (see  postscript),  I  have  added  the  times  of  maxima  and  minima 
of  Sun  spots,  as  determined  by  the  investigations  of  SCHWABE,  WOLF,  and 
others. 


By  J.  M.  Schaeberle.  77 


1851,  July  28. 

The  daguerreotype  taken  at  Konigsberg  shows  only  the  inner 
and  brighter  portions  of  the  corona.  The  resemblance  to  the 
inner  corona  of  July,  1878,  is  apparent.  As  required  by  the 
theory  for  a  typical  form,  when  ft  is  positive,  the  axis  of  the 
inner  corona  is  inclined  eastward,  according  to  the  inclination 
of  the  faint  boundaries  of  the  wings  just  visible.  (Maximum 
of  spots,  1848;  minimum,  1856.) 

1853,  November  30. 

RANYARD  gives  no  drawing  of  this  eclipse,  but  the  description 
is  just  what  the  theory  requires  it  to  be  when  the  Earth  is  near 
the  node.  (Five  years  after  maximum,  and  three  years  before 
minimum  of  spots.) 

1868,  September  7. 

The  drawing  in  general  agrees  with  the  form  required  by 
theory  when  ft  is  large.  (Compare  with  Figure  7,  Plate  I.) 
(Minimum  of  spots,  1856;  maximum,  1860.) 

1860,  July  18. 

The  photograph  by  MONSERRAT  shows  only  the  innermost 
parts  of  the  corona.  The  faint  traces  of  the  wing  boundaries 
indicate  that  the  inner  coronal  axis  is  inclined  towards  the  east, 
as  it  should  be.  The  drawings  are  very  discordant  among  them- 
selves, and  show  much  polar  extension.  The  majority  of  the 
drawings  also  give  an  eastwrard  inclination  to  the  coronal  axis. 
Many  of  the  drawings,  especially  the  grotesque  one  by  TEMPEL, 
I  can  reproduce  almost  exactly,  with  a  model.  (Maximum  of 
spots,  1860.) 

1867,  August  18. 

No  photographs;  the  one  drawing,  which  does  not  agree  with 
the  description  by  the  observer,  shows  great  equatorial  exten- 
sion, with  only  a  few  short  rays  at  the  pole.  (Minimum  of 
spots,  1867.5.) 

1868,  August  18. 

All  the  drawings  agree  in  giving  evidence  of  a  considerable 
inclination  of  the  Sun's  axis.  (Compare  the  drawings  with  the 
denser  portions  of  Figure  5,  Plate  I.)  The  majority  of  the 
drawings  give  evidence  of  an  eastward  inclination  of  the  inner 


78        A  Mechanical  Theory  of  the  Solar  Corona, 

coronal  axis  corresponding  to  a  positive  value  of  ft.     (Mini- 
mum of  spots,  1867.5;  maximum,  1870.5.) 

1869,  August  7. 

Both  the  photograph  and  the  drawing  are  in  accord  with  the 
theory.  In  the  drawing  of  MEEK  and  SCHOTT  the  extension  in 
the  equatorial  region  is  greatest  at  the  equator,  while  the  gen- 
eral outlines,  both  in  the  photograph  and  drawing,  are  quite 
similar  to  the  inner  portions  of  Figure  5,  Plate  I.  According 
to  the  boundaries  of  the  wings  as  shown  on  WHIPPLE'S  photo- 
graph, the  axis  of  the  inner  corona  is  inclined  eastward  as 
required  by  theory  when  ft  is  positive.  (Minimum  of  spots, 
1867.5;  maximum,  1870.5.) 

1870,  December  22. 

The  WILLARD  photograph  of  this  eclipse,  aside  from  the  fact 
that  the  polar  rays  and  other  fine  details  of  structure  are  wholly 
wanting,  is  strikingly  similar  to  our  Cayenne  photographs,  when 
they  are  printed  so  as  to  show  only  the  same  extent.  No  fine 
coronal  details  are  shown.  On  the  BROTHERS  photograph  the 
Sun  seems  to  have  reappeared  during  the  exposure.  The  vari- 
ous drawings  of  the  outer  corona  are  discordant  among  them- 
selves. As  required  by  theory,  when  ft  is  negative,  the  wing 
boundaries  indicate  that  the  axis  of  the  inner  corona  is  inclined 
towards  the  west.  (Maximum  of  spots,  1870.5.) 


,  December  12. 

The  four  excellent  drawings  by  DAWSON,  give  a  quadrilateral 
outline  to  the  outer  corona,  but  the  others  do  not  as  a  rule  give 
evidence  of  a  small  value  for  ft.  The  photographs  taken  at 
Baikul  and  Dodabetta,  however,  give  almost  exactly  the  same 
detail.  Practically  the  same  structure  is  shown  at  both  poles, 
so  that  a  superficial  inspection  of  the  photographs  alone  will 
not  determine  which  pole  is  turned  towards  the  Earth.  The 
boundaries  of  the  wings  extend  quite  up  to  the  poles,  so  that 
only  the  nearly  normal  rays  at  the  poles  are  shown  on  the  pho- 
tographs. At  the  time  of  this  eclipse,  the  Earth  was  nearer  to 
the  plane  of  the  Sun's  equator  than  it  was  at  any  previous  or 
subsequent  eclipse  of  which  photographs  were  obtained.  Com- 
pared with  the  equatorial  extension,  the  polar  extent  was  very 


By  J.  M.  Schaeberle.  79 

large.  The  observed  general  outline  can,  however,  be  fully  sat- 
isfied by  supposing  the  eruptive  forces  to  have  been  apparently 
more  active  near  the  superior  limits  of  the  Sun-spot  zone,  or 
that  the  equatorial  streamers  suffered  retardation  by  coming 
into  contact  with  returning  streams.  As  the  original  negatives 
were  only  three  tenths  of  an  inch  in  diameter,  considerable 
uncertainty  may  exist  in  the  fainter  outlines  of  the  enlarged 
prints.  I  was  so  fortunate  as  to  have  the  use  of  a  good  positive, 
kindly  loaned  to  me  by  Mrs.  R.  A.  PROCTOR  (evidently  made 
from  a  copy  of  the  original  negative  and  enlarged  about  three 
diameters).  I  made  a  number  of  shorter  timed  negatives,  and 
these  give,  near  the  Sun,  greater  excess. of  equatorial  extent 
and  less  of  polar  extent  than  a  positive  of  the  January  1,  1889, 
eclipse  treated  in  the  same  way,  but  the  boundaries  are  not  as 
sharply  denned  in  the  former  case  as  they  are  in  the  latter. 
From  experiments  with  a  model,  the  forms  of  the  more  lumi- 
nous confused  masses  are  so  plainly  the  result  of  apparent  inter- 
sections of  streamers  (some  of  which  are  doubtless  descending) 
that  a  more  detailed  comparison  can  be  dispensed  with,  since 
no  known  forces  could  possibly  account  for  the  various  forms 
which  can  be  traced  on  this  photograph,  if  we  suppose  the 
observed  outlines  to  represent  actual  forms  in  space.  As 
required  by  the  theory,  the  axis  of  the  inner  corona  is  nearly 
coincident  with  the  Sun's  axis,  being  slightly  inclined  towards 
the  west,  ft  having  a  negative  value.  (Maximum  of  spots, 
1870.5;  minimum,  1879.0.) 

1874,  April  16. 

There  were  no  photographs  taken  at-  this  eclipse.  It  is 
described  as  being  similar  to  the  eclipse  of  August,  1868.  As 
drawn  by  STONE,  the  axis  of  the  inner  corona,  given  by  RAN- 
YARD,  is  inclined  towards  the  west,  in  agreement  with  the  typ- 
ical form.  A  mere  drawing,  however,  is  deserving  of  but  little 
weight  so  far  as  the  location  of  this  axis  is  concerned.* 

1875,  April  6. 

This  eclipse  is  described  as  being  curiously  similar  to  the  one 
of  the  previous  year  (April  16).  The  photographs  by  LOCKYER 

*NOTE.— The  observed  data  for  comparison  between  theory  and  observation, 
up  to  and  including  this  date,  have  been  taken  from  RANYARD'S  excellent 
work  on  Solar  Eclipses. 


80 


A  Mechanical  J^heory  of  the  Solar  Corona, 


and  SCHUSTER  give  unmistakable  evidence  of  a  considerable 
inclination  of  the  Sun's  axis,  as  shown  by  the  boundaries  of  the 
wings.  The  telescopes  were  not  driven  by  clockwork,  so  that 
the  polar  rays  are  not  shown.  The  direction  of  the  Sun's  axis 
is  not  indicated  with  the  necessary  accuracy  to  determine  the 
inclination  of  the  inner  coronal  axis  with  certainty.  (Maxi- 
mum spots,  1870.5;  minimum,  1879.0.) 

1878,  July  29. 

The  first  available  photographs  on  which  the  finer  details  of 
the  structure  at  the  poles  are  of  such  a  character  as  to  permit 
of  their  being  used  to  test  the  correctness  of  the  theory  were 
obtained  at  this  eclipse.  In  the  drawing,  made  by  Professor 
HARKNESS,  from  the  photographs  obtained  at  this  eclipse,  pub- 
lished in  the  volume  issued  by  the  United  States  Naval  Observ- 
atory, the  polar  streamers  are  so  well  defined  that  I  have  been 
able  to  make  the  following  comparison  between  the  observed  (o) 
and  computed  (c)  values  of  K.  As  the  measures  are  necessa- 
rily only  approximate,  I  have  recorded  the  measured  inclina- 
tions to  the  nearest  five  degrees  for  each  ten  degrees  of  polar 
distance  available: 

1878,  July  29 — Observed  and  Computed  Values  of  K. 


DISTANCES  FROM  NEARER  POLE. 


QUADRANT. 

10° 

20° 

30° 

40° 

0 

c 

0  —  C 

0 

c 

0  —  C 

0 

c 

0  —  C 

0 

c 

0  —  C 

1. 

10° 

15° 

—5° 

30° 

31° 

1° 

40° 

46° 

—  fi° 

45° 

58° 

—13° 

II. 

10 

15 

—5 

15 

31 

16 

35 

46 

—11 

III. 

15 

15 

0 

20 

81 

11 

35 

46 

—11 

IV. 

10 

15 

—5 



The  observed  values  in  the  above  table  were  taken  from  the 
composite  drawing  (Plate  XX.,  Fig.  3),  found  in  United  States 
Naval  Observatory  publication  on  the  "  Solar  Eclipse  of  July 
29,  1878."  The  photographs  taken  at  different  stations  are  in 
accord  with  each  other.  The  numerous  drawings  are,  as  usual, 
very  discordant  among  themselves,  but  on  the  whole  indicate 
a  comparatively  large  value  of  ft.  The  northern  wings  have 


By  J.  M.  Schaeberle.  81 

multiple  boundaries  on  the  sides  towards  the  nearer  pole.  Both 
coronal  poles  are  east  of  the  Sun's  poles;  but  the  line  joining 
the  poles  of  the  corona,  as  found  by  means  of  the  boundaries  of 
the  wings  adjacent  to  the  poles,  is  inclined  towards  the  east,  as 
required  for  a  typical  form.  The  polar  rays,  alone  considered, 
would'  indicate  that  the  coronal  axis  was  nearly  parallel  to  the 
Sun's  axis.  Professor  HARKNESS  calls  attention  to  the  fact  that 
the  orientation  may  be  several  degrees  in  error,  as  only  the 
sides  of  the  photographic  plates  could  be  used  as  guides. 

The  excellent  drawing  by  TROUVELOT  is  in  remarkable  agree- 
ment with  the  photographs.  Naked-eye  drawings  by  Professor 
NEWCOMB  and  Professor  LANGLEY,  the  latter  being  stationed  on 
the  top  of  Pike's  Peak,  show  the  greatest  equatorial  extent  of 
the  corona  that  has  been  observed  'up  to  the  present  time. 
(Compare  the  drawing  made  from  the  photographs  with  Figure 
5,  Plate  VI.)  (Minimum  of  spots,  1879.0.) 

1880,  January  11. 

The  sketches  made  during  this  eclipse  show  how  untrustwor- 
thy the  data  derived  from  mere  drawings  can  be.  In  Professor 
DAVIDSON'S  Report  (see  United  States  Coast  and  Geodetic  Sur- 
vey Report  for  1882),  the  corona  is  outlined  as  in  Figure  2  or 
3,  Plate  VI.,  while  in  the  sketches  of  Lieutenant  CHRISTOPHER 
only  a  narrow,  nearly  concentric  band  of  light  is  shown  sur- 
rounding the  dark  limb  of  the  Moon.  There  are  no  photo- 
graphs of  this  eclipse,  so  far  as  known. 

1882,  May  '17. 

The  drawing,  made  from  photographs,  given  in  Captain  AB- 
NEY'S  and  Dr.  SCHUSTER'S  report  on  the  solar  eclipse,  is  exceed- 
ingly interesting  as  representing  an  arrangement  of  streamers 
similar  to  the  conditions  found  in  the  model;  that  is,  no  polar 
rays  are  formed.  The  general  appearance  of  the  nearly  circular 
outline  of  the  corona  would  seem  to  indicate  that  the  solar 
activity  was  considerable  in  the  higher  limits  of  the  spot-zones; 
or,  what  is  more  probable,  that  those  in  the  middle  latitudes 
were  retarded,  and  that  the  incoming  streamers  were  more 
numerous  at  the  equator  (see  Postscript),  and  that  in  both 
zones  only  the  more  conspicuous  streamers  of  the  farther  hemi- 
sphere are  seen  in  projection  through  the  dense  masses  of 

6  t^^  *ry&t*,*s>^-? 

r     ' 
,-/ Ai,  //?**!/  ,     £%*«:,/. 


82        A  Mechanical  Theory  of  the  Solar  Corona, 


rays,  most  of  which  are  apparently  wholly  formed  in  the  nearer 
hemisphere.  There  is  strong  evidence  tending  to  show  that 
there  were  numerous  collisions,  as  in  many  places  the  corona 
is  brightest  at  some  distance  from  the  Moon's  outline.  I  can 
almost  exactly  reproduce  this  coronal  form  with  a  model.  The 
inner  portions  of  Figure  2,  Plate  VI.,  are  quite  suggestive. 
(Minimum  of  spots,  1879;  maximum,  1883.) 

1888,  May  6. 

The  drawings  made  by  Professor  TACCHINI  and  Dr.  DIXON  give 
evidence  of  a  considerable  inclination  of  the  Sun's  axis.  The 
Lick  Observatory  does  not  possess  any  photographs. 

Note — October,  1890. — Since  the  above  was  written  the  1889 
volume  of  the  "  Philosophical  Transactions"  has  been  received. 
Like  the  previous  eclipse  (1882)  there  is  much  confusion  in  the 
coronal  detail.  If  the  orientation  of  the  enlarged  drawing  made 
from  photographs  secured  by  the  English  party  is  correct  as 
published  in  this  volume,  then  we  have  here  a  case  of  a  nearly 
circular  corona,  in  which  the  less  inclined  streamers  projected 
near  the  north  pole  of  the  Sun  had  a  decidedly  greater  density 
than  the  more  inclined  ones;  since  the  apparent  north  coronal 
pole  is  at  the  enormous  distance  of  nearly  20°  to  the  east  of  the 
Sun's  pole!!  At  the  south  pole  the  structure  is  more  nearly 
radial,  so  that  the  position  of  the  south  coronal  pole  can  not  be 
located  with  great  accuracy. 

Note  No.  2 — March,  1891. — Since  the  above  has  been  in  type 
I  have,  very  fortunately,  found  a  photographic  print  of  this 
eclipse  (see  Annuaire,  Bureau  des  Longitudes,  1884),  made  by 
M.  JANSSEN  from  a  negative  which  he  exposed  during  the  whole 
time  of  totality.  Although  the  orientation  can  only  be  made 
by  means  of  the  edges  of  the  card  on  which  the  print  is  mounted 
(the  north  pole  is  toward  the  lower  left-hand  corner  of  the 
card),  still  all  doubt  as  to  the  proper  orientation  of  the  above 
mentioned  drawings  seems  to  be  removed.  Dr.  DIXON  observed 
with  a  diagonal  eye-piece;  the  top  of  his  drawing  should  there- 
fore be  marked  S.  instead  of  N. 

In  Mr.  WESLEY'S  drawing  (Phil.  Trans.)  the  top  of  the  page 
is  N.  The  axis  is  correctly  orientated. 

The  remarkable  difference  which  can  exist  between  the  draw- 
ing of  a  photograph  taken  with  one  instrument  and  a  photo- 
graphic print  from  a  negative  taken  with  another  instrument  is 


By  J.  M.  Schaeberle. 


83 


well  illustrated  in  this  case.  In  JANSSEN'S  print  not  only  are 
the  symmetrical  wings  and  fish  tails  shown,  but  even  the  trumpet- 
shaped  outlines,  on  the  east  side  at  least,  are  unmistakable.  The 
extended  luminosity  near  the  north  pole  would  seem  to  indicate 
that  the  streamers  were  not  uniformly  distributed  in  longitude, 
so  that  the  ratio  of  D  to  D'  is  no  longer  that  which  holds  good  for  a 
typical  corona.  Now,  comparing  Mr.  WESLEY'S  drawing  with 
the  print,  an  apparent  tendency  to  form  two  north  and,  less 
conspicuously,  two  south  coronal  poles  adjacent  to  the  bound- 
aries of  the  wings  is  at  once  recognized.  The  reversal  of  the 
inclinations  near  the  north  pole  is  very  marked  and  is  due  to 
an  irregular  variation  in  the  density  of  the  streamers,  as  can  be 
readily  shown  with  the  aid  of  the  models  (see,  for  instance, 
Plate  VII.,  Fig.  a).  The  tendency  to  form  multiple  poles  is 
also  partially  shown  in  some  of  the  figures  of  Plate  VI. 

The  axis,  which  is  symmetrically  situated  with  reference  to 
these  poles,  in  Mr.  WESLEY'S  drawing,  is  inclined  towards  the 
west,  in  agreement  with  the  theory.  Compare  the  print  with 
Figures  3,  4,  and  6  of  Plate  VI.,  disregarding  the  unsymmetrical 
luminosity  above  the  north  pole.  (Maximum  of  spots,  1883.) 

1886,  August  29. 

The  photographs  taken  by  PICKERING  on  the  Island  of  Gre- 
nada show  enough  of  the  finer  detail  in  certain  places  near  the 
poles  to  allow  of  a  rough  comparison  between  theory  and  obser- 
vation. The  inclinations  (to  the  nearest,  5°)  of  the  polar  rays 
to  normals  through  their  bases  are  given  in  the  table  below  for 
each  10°  of  polar  distance  applicable.  The  measures  are  made 
from  the  drawing  given  in  the  frontispiece  of  Harvard  College 
Observatory  Annals,  Vol.  XVIII.,  No.  V. 


DISTANCE  FROM  NEARER  POLE. 


QUADRANT. 

10° 

20° 

30° 

40° 

0 

c 

o—  c 

0 

c 

o—  c 

0 

c 

o  —  c 

0 

c 

0  —  C 

I. 

15° 

15° 

0° 

25° 

31° 

6° 

II. 

15 

15 

o 

20 

31 

—11 

50° 

46° 

4-4° 

III. 

10 

15 

—5 

IV. 

? 



84        A  Mechanical  Theory  of  the  Solar  Corona, 


In  the  second  quadrant,  at  30°  polar  distance,  the  rays  are 
not  distinct,  being  nearly  lost  in  the  general  illumination;  the 
measure  is  therefore  unreliable.  Just  at  the  south  pole  there  is 
a  cone  with  the  sides  inclined  10°  to  the  normal,  apparently 
made  by  the  overlapping  of  rays.  On  the  west  side  of  the  north 
pole  the  distribution  of  the  streamers  is  apparently  too  irregu- 
lar to  produce  even  a  trace  of  the  symmetrical  inclined  rays; 
this  supposition  is  further  strengthened  by  the  fact  that  at  25° 
polar  distance  there  is  a  great  wing  extending  to  a  distance 
nearly  equal  to  the  equatorial  extent  of  the  corona.  As  required 
by  the  theory  when  ft  is  positive,  the  axis  of  the  inner  corona 
is  inclined  towards  the  east.  (Maximum  of  spots,  1883;  mini- 
mum, 1888  or  1889.) 

Note — October,  1890. — Since  the  above  was  written  the  volume 
of  the  PhiL  Trans.,  which  contains  a  drawing  of  a  photograph 
of  this  corona  (discussed  by  Messrs.  DARWIN,  SCHUSTER,  and 
MAUNDER),  has  appeared.  The  orientation  differs  something 
less  than  4°  from  the  PICKERING  photograph,  so  that  for  this 
copy  of  the  corona  the  coronal  axis  is  slightly  inclined  west- 
ward. The  following  measures  can  be  compared  with  those  in 
the  preceding' table: 


QUADRANT. 

DISTANCE  FROM  NEARER  POLE. 

10° 

20° 

30° 

40° 

0 

c 

o  —  c 

0 

c 

0  —  C 

0 

c 

0  —  C 

0 

c 

0  —  C 

I.  . 

20° 
20 
10 
0 

15° 
15 
15 
15 

+  5° 

It 

—15 

40° 
30 
20 
20 

31° 
31 
31 
31 

±r 

—11 
—11 

II. 

50° 

46° 

^° 

III.  .. 

IV  .  

1 

If  the  orientation  is  changed  so  as  to  agree  with  PICKERING'S 
diagram,  the  above  residuals  will  be  reduced  in  magnitude  some- 
what. 

1887,  August  18-19. 

The  best  photographs  taken  at  Jourgewetz  by  Dr.  BELOPOLSKY 
are  similar  to  those  of  the  previous  year.  A  certain  con- 
fusion is  apparent,  so  that  no  great  amount  of  detail  is  shown 
at  the  poles.  The  axis  of  the  inner  corona  apparently  had  a 


By  J.  M.  Schaeberle. 


85 


decided  inclination  toward  the  east,  as  required  by  the  theory 
when  ft  is  positive.  Dr.  GLASENAPP'S  results  give  the  same  evi- 
dence. ( Minimum *of  Sun  spots,  probably  1888  or  1889.) 

1889,  January  1. 

It  is  no  exaggeration  to  say  that  the  photographs  taken  dur- 
ing this  eclipse  are  better  than  any  which  had  previously  been 
taken.  On  the  magnificent  negatives  secured  by  BARNARD, 
BURCKHALTER,  CHARROppiN,  Harvard  College  Observatory 
party,  and  others,  the  coronal  structures  are  shown  in  a  way 
that  leaves  but  little  to  be  desired. 

In  the  following  table  the  comparison  between  theory  and 
observation  will  prove  interesting: 


DISTANCE  FROM  NEARER  POLE. 


QUADRANT. 

10° 

20° 

30° 

40° 

0 

c 

o  —  c 

0 

c 

0  —  C 

; 

0 

c 

o  —  c 

0 

c 

o  —  c 

I 

20° 

15° 

4-5° 

30° 

31° 

1° 

35° 

46° 

-  11° 

50° 

58° 

8° 

II. 

20 

15 

4-5 

Ill  

10 

15 

±5 

25 

31 

—6 

IV. 

10 

15 

—  5 

25 

BJ 

-6 

I  have  only  used  those  polar  distances  at  which  the  indi- 
vidual rays  could  still  be  recognized.  The  corona  was  nearly 
of  the  typical  form.  The  great  equatorial  extension  with  the 
trumpet-shaped  outlines  has  just  the  form  which  streamers 
of  indefinite  length  from  low  latitudes  will  produce  in  pro- 
jection. With  the  increase  of  distance  the  illumination 
gradually  fades  out,  but  towards  the  axes  of  greatest  den- 
sity in  projection  the  increasing  number  of  overlapping 
streamers  causes  a  gradual  increase  in  the  illumination,  result- 
ing in  the  trumpet-shaped  outlines  which  form  so  promi- 
nent a  feature  of  this  eclipse.  For  all  coronas,  in  which  the 
fish  tails  are  prominent,  this  particular  feature  should  here- 
after be  shown  in  cases  where  the  observers  are  favored  with 
exceptionally  good  atmospheric  conditions.  This  was  the  case 
for  the  present  eclipse;  the  clear  California  sky  revealed  out- 
lines not  before  seen  on  photographs  taken  during  sun-spot 
minima. 


86 


A  Mechanical  Theory  of  the  Solar  Corona, 


Not  only  is  this  phenomenon  a  necessary  consequence  of  the 
theory,  but  all  doubt  as  to  its  nature  would  seem  to  be  removed 
by  the  appearance  of  the  photographs  themselves;  numerous 
streamers,  of  such  a  length  and  form  as  to  preclude  the  idea 
that  they  coincide  with  magnetic  lines  of  force,  are  seen  radiat- 
ing from  parts  of  the  Sun's  limb,  which  indicate  that  the 
origins  are  in  the  low  latitudes.  Here,  again,  the  model  need 
only  be  compared  with  the  photographs,  to  test  the  agreement 
of  the  theory  with  observation.  The  boundaries  of  the  wings 
in  the  southern  hemisphere  are  multiple  on  the  sides  turned 
toward  the  nearer  pole.  The  axis  of.  the  inner  corona,  as 
required  by  the  typical  form,  is  inclined  toward  the  west,  the 
Earth  being  below  the  Sun's  equator.  (Minimum  of  spots, 
1888  or  1889.) 

1889,  December  21,  22. 

The  photographs  taken  at  Cayenne  again  show  the  structure 
of  the  corona  with  such  minuteness  of  detail  that  a  direct  com- 
parison between  the  observed  and  theoretical  inclinations  of  the 
polar  rays  can  also  be  used  to  test  the  theory. 

As  the  position  of  the  meridian  is  not  indicated  on  the  prints, 
the  photographs  can  be  accurately  orientated  by  means  of  the 
following  datum.  The  center  of  the  heaviest  north  polar  ray 
(the  most  westerly  one  of  the  more  conspicuous  and  nearly 
normal  rays)  has  a  position  angle  of  4°. 8;  the  pole  of  the  Sun 
is  therefore  2°  east  of  the  heavy  north  polar  ray. 


DISTANCE  FROM  NEARER  POLE. 


QUADRANT. 

10° 

20° 

30° 

40° 

0 

c 

o  —  c 

o 

0—  C 

o 

c 

0—  C 

0 

c 

0  —  C 

1 

10° 

15° 

—5° 

20° 

31° 

—11° 

40° 

46° 

—6° 

11 

10 

15 

—  5 

III 

20 

15 

-j_5 

25 

31 

—  6 

45 

46 

—  1 

IV 

20 

15 

4-5 

35 

31 

4-  4 

45 

46 

—  1 

| 

Although  the  sky  was  apparently  free  from  clouds  during  the 
total  phase  of  the  eclipse,  the  air  was  so  charged  with  moisture 
that  the  atmospheric  glare  must  have  been  very  prominent. 
Yet,  notwithstanding  these  conditions,  the  equatorial  extent  of 
the  corona,  as  shown  on  the  photographs,  is  more  than  a  degree; 


By  J.  M.  Schaeberle.  87 

the  wings  are  very  conspicuous,  and  the  polar  rays  are  shown 
with  all  desired  distinctness.  The  trumpet- shaped  outlines,  so 
prominent  a  feature  in  the  previous  eclipse,  are  lost  in  the  sky 
illumination,  although  faint  traces  of  this  phenomenon  can  be 
distinguished. 

In  the  southern  zone  there  was  evidently  a  vigorous  outburst 
near  longitude  r — r0— 0°.  The  protuberances  (shown  on  the 
negatives)  projected  at  this  part  of  the  Moon's  outline  give 
evidence  to  the  same  effect.  The  boundaries  of  the  wings  in 
the  southern  hemisphere  are  multiple  on  the  sides  turned 
towards  the  nearer  pole. 

As  required  by  the  theory,  the  axis  of  the  inner  corona  is 
inclined  slightly  towards  the  west,  the  Earth  being  below  the 
Sun's  equator.  (Minimum  of  spots,  1888  or  1889.) 

Probable  Form  of  the  Solar  Coronas  of  1892  and  1893. 

The  next  total  eclipse  of  the  Sun  takes  place  in  1892,  April 
26.  If  observed,  the  following  prediction  as  to  its  form  should, 
in  general,  be  verified,  under  favorable  atmospheric  conditions: 
Polar  extent  large.  Inner  coronal  axis  (if  polar  rays  or 
wings  are  shown)  inclined  westward.  Rifts  numerous.  Indi- 
cations of  collisions.  General  form  similar  to  Figure  7,  Plate 
VI.  The  same  description  will  apply  to  the  eclipse  of  April 
15-16,  1893. 

It  will  be  noticed  that  I  have  used  the  same  constants  for 
finding  the  value  of  k  for  a  given  p  in  all  cases  (see  page  75). 
A  closer  agreement  between  theory  and  observation  could  doubt- 
less have  been  obtained  by  varying  the  values  of  c  and  a  (for 
different  values  of  /?)  ancT  taking  into  account  the  shifting  of  the 
coronal  pole;  but  as  it  appeared  that  the  measured  inclinations 
were  liable  to  errors,  which  as  a  rule  much  exceeded  those  due  to 
neglecting  the  terms  which  involved  or  cjaused  the  shifting  of 
the  coronal  poles,  I  deemed  it  best  to  refer  all  measures  to  the 
Sun's  true  poles.  The  magnitude  of  the  residuals  obtained  can 
then  be  used  to  detect  any  abnormal  discrepancies  which  may 
result  from  some  error  in  the  orientation  of  the  photograph. 

The  object  of  the  present  investigation  was  not  to  force  an 
exact  agreement  by  the  arbitrary  variation  of  certain  quanti- 
ties, but  to  secure  confirmatory  or  non-confirmatory  evidence, 


88        A  Mechanical  Theory  of  the  Solar  Corona, 

by  comparing  a  purely  theoretical  investigation  of  a  general 
character  with  the  results  obtained  from  actual  observation. 

It  is  hardly  necessary  to  state  that  nothing  in  this  theory 
requires  that  all  the  streamers  shall  be  confined  between  any 
fixed  circles  of  latitude,  nor  that  the  apparent  density  and 
magnitude  of  the  streamers  may  not  be  subject  to  periodic 
variations,  due  to  physical  causes  which  relate  to  the  molecular 
nature  of  the  Sun's  internal  constitution,  with  which  this  in- 
vestigation has  nothing  to  do.  (See  Postscript.) 

There  seems  to  be  no  feature  of  the  coronal  structure  ivhich 
cannot  be  accounted  for  in  a  satisfactory  manner  by  this  new  theory 
of  the  solar  corona. 

In  conclusion,  it  gives  me  pleasure  to  thank  Messrs.  BURN- 
HAM  and  BARNARD  for  their  aid  in4  the  work  of  the  photographic 
reproductions,  and  Mr.  KEELER  for  various  information  relating 
to  spectroscopic  solar  physics. 

I  am  much  indebted  to  Professor  HOLDEN,  who,  during  the 
preparation  of  this  memoir,  has  ever  been  ready  to  aid  me  in 
various  ways. 

MT.  HAMILTON,  June,  1890. 

J.  M.  SCHAEBERLE. 


POSTSCRIPT. 

I  have  spent  some  time  in  an  extended  examination  of  the 
magnificent  spectroscopic  observations  made  at  Rome,  with  a 
view  to  determine,  if  possible,  whether  the  solar  prominences 
observed  in  high  latitudes  could  not  bareconciled  to  the  hypoth- 
esis that  they  were  but  the  projections  of  streams,  which,  issu- 
ing from  a  low  latitude,  appeared  in  projection  to  come  from 
the  limb  of  the  Sun.  In  many  instances  this  seems  to  be  the 
case,  but  the  complications,  especially  in  the  low  latitudes, 
resulting  from  the  perspective  overlapping  of  these  promi- 
nences in  largely  different  longitudes,  is  so  great  that  much 
uncertainty  exists  as  to  the  motion  of  any  given  prominence. 
The  uncertainty  could  be  settled  at  once  by  following  a  con- 
spicuous polar  prominence  for  several  hours,  and  carefully 
recording  its  position-angle  from  time  to  time.  If  the  base  of 
such  a  prominence  is  in  a  low  latitude,  the  position-angle 


By  J.  M.  Schaeberle.  89 

should  change  at  the  rate  of  about  2°  an  hour.  I  have  not 
had  an  opportunity  to  make  an  observation  of  this  kind  since 
the  theoretical  investigation  was  completed. 

The  prominences  at  the  poles  are  so  rare,  and  the  observa- 
tions usually  so  short,  that  no  definite  conclusions  can  be  drawn 
from  the  data  at  hand.  Again,  prominences  at  the  poles  should, 
on  this  hypothesis,  always  have  large  component  velocities  either 
towards  or  away  from  the  Earth. 

During  the  total  eclipse  of  August  29,  1886,  Professor  SCHUS- 
TER observed  the  spectrum  of  a  great  prominence  near  the  pole 
of  the  Sun.  His  observations  indicated  a  motion  of  two  hun- 
dred and  forty-seven  miles  per  second  towards  the  observer. 
Assuming  the  origin  of  the  prominence  to  be  in  the  spot-zone, 
this  velocity  indicates  roughly  an  initial  parabolic  velocity. 

As  bearing  upon  this  point,  the  following  extracts  from 
"  Chemistry  of  the  Sun,"  by  that  eminent  solar  physicist,  J. 
NORMAN  LOCKYER,  will  be  found  very  suggestive.  The  italics 
are  my  own: 

Such  prominences  have  been  seen  to  mount  upwards  at  the  rate  of  250 
miles  a  second  ;  that  is,  nearly  1,000,000  miles  an  hour.  *  *  *  There 
are  indications  that  these  prominences,  instead  of  rising  vertically,  as  we  may 
imagine  them  to  do,  are  at  times  shot  out  sideways — almost  tangentially.  In  that 
case,  of  course,  the  spectroscope  enables  us  to  determine  the  velocity.  One 
hundred  miles  a  second,  either  towards  or  from  the  eye,  is  by  no  means  an  uncommon 
velocity.  *  *  *  The  height  of  some  of  these  prominences  is  very  great. 
Professor  YOUNG  records  one  seen  in  1878  as  being  nearly  400,000  miles  high ; 
that  is,  13|  minutes  of  arc.  the  solar  radius  being  16  minutes. 

The  actual  velocity  of  motion  will,  in  general,  always  be 
greater  than  the  observed,  since  the  spectroscope  only  gives 
that  component  which  is  parallel  to  the  Earth's  radius- vector, 
while  the  direct  visual  observation  only  gives  the  component 
at  right  angles  to  the  same  line. 

The  small  inclined  saw-tooth  protuberances,  as  well  as  many 
of  the  grotesque  larger  ones,  are  probably  formed  in  much  the 
same  way  that  the  polar  rays  are  produced;  the  sudden  changes 
of  inclination  being  due  to  variations  in  the  density  of  the 
streams.  It  would  seem  to  require  a  continuous  and  more  or 
less  uniform  series  of  eruptions  in  certain  zones  on  the  solar 
surface  to  satisfactorily  account  for  these  ever-present  smaller 
protuberances,  and  the  theory  certainly  demands  such  a  dis- 
tribution of  the  streamers.  Let  us  now  consider 


90        A  Mechanical  J^heory  of  the  Solar  Corona, 

SOME   PHYSICAL    PHENOMENA    INVOLVED    IN    THE    MECHANICAL 
THEORY  OF  THE  CORONA. 

While  I  invite  the  severest  criticism,  from  astronomers,  of  the 
theory  given  in  the  preceding  pages,  I  ask  their  indulgence  with 
reference  to  certain  deductions  which  I  have  made,  and  now, 
with  great  deference,  submit  to  their  attention.  Assuming  my 
premises  (The  Mechanical  Theory)  to  be  true,  I  trust  that  in 
deducing  some  of  the  resulting  phenomena  my  arguments  will 
at  least  be  found  to  have  a  logical  sequence. 

All  the  results  obtained  in  the  foregoing  investigation  have 
been  deduced  on  the  hypothesis  that  the  force  of  ejection  is 
such  as  to  give  a  parabolic  velocity  to  the  streams;  but  so  far 
as  the  form  near  the  Sun  is  concerned,  an  inspection  of  Table  I. 
at  once  shows  that  practically  the  same  results  would  be  obtained 
on  the  hypothesis  that  the  force  is  only  just  sufficient  to  give  an 
elliptical  velocity  corresponding  to  a  period  of  only  a  few  hours. 

The  moment  the  returning  streams  are  taken  into  consider- 
ation the  effect  is  such  as  to  cause  a  periodic  variation  in  the 
detail  of  the  corona,  and  simultaneously  to  cause  a  periodic  vari- 
ation in  the  surface  features  of  the  Sun,  as  I  shall  now  proceed 
to  show. 

To  whatever  cause  the  eruptions  in  certain  zones  on  the 
Sun  may  be  due,  we  are  evidently  justified  in  assuming  that, 
in  the  long  run,  the  forces  there  at  work  have,  at  a  given  period 
of  the  Sun's  age,  a  mean  value  (F).  One  measure  of  this  force 
(F)  will  be  the  maximum  distance  (d)  from  the  Sun's  center 
(=2a  nearly),  to  which  a  given  particle  (mass=m)  is  projected 
in  the  time  \t  (nearly),  so  that  the  periodic  time  will  be  t.  As 
has  already  been  shown,  the  heliocentric  latitude  of  an  ejected 
particle  during  its  whole  motion  will  remain  nearly  the  same, 
so  that  the  latitudes  of  different  parts  of  the  same  stream  will 
be  nearly  the  same  as  the  latitude  of  the  point  of  ejection.  Now, 
if  each  stream  of  particles  in  a  given  zone  is  ejected  by  an 
instantaneous  force  (F),  the  more  advanced  portions  of  the 
streams  will  be  unimpeded  during  the  first  half  of  their  path; 
on  returning,  however,  the  chance  of  collision  with  the  same  or 
other  outgoing  streams  varies  inversely  as  the  square  of  the 
distance  from  the  Sun. 

Near  the  Sun,  therefore,  collisions  must  occur  which  tend  to 


By  J.  M.  Schaeberle.  91 

retard  or  stop  the  outgoing  streams,  resulting  in  a  temporary 
increase  in  the  heat  pf  the  combined  colliding  masses  (causing 
a  consequent  increase  in  the  brightness  of  the  corona  at  such 
places,  and  at  the  same  time  rendering  the  coronal  detail  more 
confused).  This  heat  will  tend  to  be  largely  dissipated  before 
such  masses  fall  back  into  the  Sun,  which  they  will  then  reach 
with  comparatively  small  velocity  and  low  temperature.  Unre- 
tarded  returning  streams  on  striking  the  Sun  will  tend  to  greatly 
raise  the  temperature  at  the  points  of  impact;  perturbed  return- 
ing streams  could,  of  course,  strike  all  parts  of  the  Sun's  surface, 
but  the  general  tendency  of  these  perturbations  will  be  to  dimin- 
ish the  latitudes  of  the  returning  streams.  Unperturbed  return- 
ing streams  will  always  fall  within  the  limits  of  the  Sun-spot 
zones. 

So  long  as  the  incoming  streams  are  very  numerous,  the  out- 
going ones  will,  in  a  great  measure,  be  stopped,  so  that,  after 
the  interval  t,  there  will  be  comparatively  few  returning  streams; 
a  direct  consequence  of  this  state  of  things  is  to  allow  free  pas- 
sage for  the  outgoing  streams,  which,  since  there  are  now  but 
few  collisions,  results  in  ( 1 )  an  apparent  diminution  in  the 
brightness  of  the  corona,  (2)  more  regular  and  sharply  denned 
detail,  and  (3),  in  general,  a  more  uniformly  illuminated  solar 
surface  (i.  e.,  fewep*  solar  spots). 

The  periodic  character  of  this  phenomenon  can  be  well  illus- 
trated by  means  of  a  vertical  jet  of  water.  When  the  water  is 
first  turned  on  it  almost  instantly  shoots  up  to  its  maximum 
height;  the  returning  drops  then  gradually  check  the  velocity 
of  the  stream  near  the  origin,  so  that  after  a  moment  the  whole 
mass  seems  to  be  piled  up  just  a  little  above  the  orifice;  before 
the  last  portions  of  the  still  falling  stream  reach  the  retarded 
stream  the  jet  begins  to  resume  its  former  activity,  and  then 
again  rises  to  a  considerable  height.  These  oscillations  are 
repeated  at  nearly  uniform  intervals,  the  period  of  one  complete 
phase  being  roughly  equal  to  twice  the  time  required  for  a  given 
drop  to  describe  the  whole  path. 

If  the  ejective  force  is  such  as  to  make  t  about  five  years,  a 
complete  cycle  of  changes  will  take  place  in  the  time  2£,  and 
after  the  same  manner  as  is  observed  in  the  Sun-spot  cycle.  It 
is  rather  remarkable  that  the  aphelion  distance  of  the  streams 
corresponding  to  this  value  of  t  is  nearly  the  same  as  Jupiter's 


92        A  Mechanical  Theory  of  the  Solar  Corona, 


distance  from  the  Sun;  so  that  the  perturbations  produced  by 
this  planet  may  have  more  to  do  with  the  regularity  of  the 
period  than  the  assumed  constant  force  of  ejection.  The  initial 
velocity  required  to  just  carry  a  particle  from  the  Sun  to  Jupiter 
is  but  little  less  than  a  parabolic  velocity.  For  an  initial  para- 
bolic velocity  Saturn,  alone  considered,  would,  on  the  same 
hypothesis,  cause  a  complete  cycle  of  less  marked  changes  in 
twenty  years,  Uranus  in  sixty  years,  and  Neptune  in  one  hun- 
dred and  twenty  years.  The  comparatively  insignificant  plan- 
ets inside  of  the  orbit  of  Jupiter  would  cause  minor  variations, 
corresponding  to  cycles,  which,  even  for  Mars,  would  be  of  less 
than  two  years'  duration. 

A  maximum  of  Sun  spots  will  therefore  correspond  to  the 
times  when  the  returning  streams  are  most  numerous;  the 
corona  at  these  same  times  will  be  brightest  and  most  con- 
fused near  the  Sun,  and  on  account  of  the  retardations,  the 
equatorial  extent  will,  as  a  rule,  be  least.  But  at  the  equator 
there  will  be  more  returning  than  outgoing  streams  (on  account 
of  the  planetary  perturbations)  ;  consequently,  the  illumination 
in  this  plane  will  be  greater  at  this  time  than  it  is  when  only 
outgoing  streams  are  present. 

A  minimum  of  Sun  spots  will  correspond  to  the  times  when 
the  incoming  streams  have  been  exhausted.  Consequently, 
the  unimpeded  outgoing  streams  will  have  their  normal  veloc- 
ity and  extent,  the  corona  will  show  great  equatorial  extension, 
and,  as  a  rule,  be  more  sharply  defined  and  have  more  promi- 
nent fish-tail  outlines,  especially  when  the  Earth  is  near  the 
Sun's  equator. 

In  the  equation: 

F 


V  increases  as  M  diminishes.  As  it  is  probable  that  at  the 
instant  of  ejection  the  masses  are  of  a  gaseous  character,  the 
velocity  may  be  very  great  without  necessarily  requiring  an 
improbable  ejective  force.  It  may  be  well  to  call  attention  to 
the  fact  that  the  initial  velocity  required  to  send  a  particle  to  a 
distance  of  only  one  solar  diameter  from  the  Sun's  surface  is 
already  greater  than  four  fifths  of  the  velocity  required  to  send 
the  same  particle  to  an  infinite  distance.  For  lines  of  motion 


By  J.  M.  Schaeberle.  93 


which  are  not  normal  to  the  Sun's  surface,  much  greater  initial 
velocities  will  be  required  to  carry  the  particles  to  the  same 
distance. 

On  this  hypothesis  the  duration  of  the  Sun-spot  period  there- 
fore indicates  that  the  forces  of  ejection  are  such  as  to  give  the 
streams  a  mean  velocity  but  little  less  than  that  in  a  parabolic 
orbit.  Streamers  having  inclined  initial  directions  of  motion 
will,  as  a  rule,  either  be  destroyed  by  others,  or  be  so  scattered 
that  no  marked  effects  will  be  produced  by  them.  (The  zone 
of  maximum  Sun  spots  is. the  same  as  the  zone  above  which  the 
maximum  number  of  collisions  takes  place.)  As  the  Earth's 
maximum  distance  from  the  plane  of  the  Sun's  equator  is  less 
than  8°,  and  as  the  zone  of  maximum  activity  on  the  Sun  has 
twice  this  latitude,  the  chance  of  the  Earth  passing  through 
an  outgoing  stream  is  less  than  it  is  for  an  incoming  (perturbed) 
stream.  Such  encounters  must,  however,  take  place. 

THE  ZODIACAL  LIGHT  AND  THE  GEGENSCHEIN. 

According  to  the  Mechanical  Theory,  the  ejected  streams  of 
matter,  although  they  are  of  double  curvature,  will  always  be 
directed  nearly  towards  the  Sun  (except  at  aphelion).  Let  us 
now  consider  some,  phenomena  which  can  be  produced  experi- 
mentally. The  diffused  light  caused  by  a  series  of  nearly 
parallel  luminous  lines  (of  indefinite  extent)  very  distant  from 
the  observer  will  always  be  most  conspicuous  in  those  direc- 
tions in  which  the  lines  are  projected  as  mere  points.  If  the 
observer  is  placed  within  the  space  through  which  these  lines 
pass,  there  will  be  two  points  of  equal  maxima  180°  apart; 
but  if  the  actual  intrinsic  brilliancy  of  the  lines  increases 
from  one  extremity  of  the  set  to  the  other,  then,  of  course,  the 
two  maxima  will  differ  enormously  in  brilliancy.  If  the  depth 
of  these  lines  in  cross-section  is  the  same  on  all  sides  of  the 
observer,  the  illumination  will  be  symmetrically  arranged  in 
concentric  zones,  which  gradually  decrease  in  brightness  as  the 
angular  distance  from  their  common  pole  (which  corresponds 
to  the  brighter  maximum)  increases,  until  the  angular  distance 
is  reached  at  which  the  apparent  increase  in  brilliancy  due  to 
projection  more  than  compensates  for  the  decrease  in  brilliancy 
due  to  distance  from  the  origin.  If  one  diameter  of  the  cross- 
section  at  the  observer  is  greater  than  any  other,  the  excess  in 
depth  produces  an  apparent  increase  of  illumination  in  a  plane 


94       A  Mechanical  Theory  of  the  Solar  Corona, 

which  contains  this  diameter  and  the  vanishing  points  of  the 
lines,  the  law  of  variation  of  brightness  in  this  plane  being  the 
same  as  for  a  circular  cross-section.  If  the  observer  is  near, 
but  not  within,  the  space  traversed  by  the  lines  of  indefinite 
extent,  no  conspicuous  variations  will  be  apparent,  although 
one  hemisphere  will  actually  be  brighter  than  the  other.  If 
in  each  of  the  above  cases  the  luminous  lines  be  assumed  to 
radiate  from  a  common  center,  which  is  at  a  great  distance  from 
the  point  of  observation,  the  distribution  of  those  lines  which 
pass  nearest  to  the  observer  will,  on  account  of  their  small 
distance,  almost  wholly  determine  the  form  of  the  resulting 
phenomenon. 

Let  us  now  consider  the  phenomenon  caused  by  the  outgoing 
and  incoming  streamers  from  the  Sun.  In  December  and  June 
the  Earth  is  in  the  plane  of  the  Sun's  equator  and  at  its  maxi- 
mum distance  from  the  nearest  zone  of  streamers,  and  it  is 
symmetrically  situated  with  reference  to  both  zones.  Now, 
since  the  Earth  is  in  neither  of  these  zones,  no  great  contrasts 
of  light  will  be  produced  on  the  side  opposite  to  the  Sun.  Even 
if  there  were  no  streamers  near  the  Earth,  the  light  in  the 
two  hemispheres  would  be  so  diffused  (covering  the  whole  visible 
sky  with  the  exception  of  an  ill-defined  less  luminous  band 
along  the  ecliptic)  that  it  is  quite  probable  the  variations  in 
light  would  not  be  apparent,  except  at  the  time  of  an  eclipse  of 
the  Sun,  when  typical  coronal  forms  would  be  seen.  But  the 
arrangement  of  the  comparatively  few  streamers  which  pass 
near  the  Earth  on  all  sides  will,  on  account  of  their  nearness, 
now  determine  the  resulting  form  of  the  outlines.  The  density 
in  projection  will  evidently  be  greatest  in  the  plane  of  the  Sun's 
equator,  but  this  density  will  be  at  a  minimum. 

When  the  Earth  is  at  its  greatest  distance  above  (September) 
or  below  (March)  the  plane  of  the  Sun's  equator,  it  will  be  at 
its  least  distance  from  the  zone  of  maximum  density  of  the 
streamers.  In  projection,  the  density  will  now  be  greatest  in 
a  plane  which  is  practically  coincident  with  the  plane  of  the 
ecliptic;  the  excess  of  streamers  in  the  direction  of  maximum 
density  will,  however,  have  a  tendency  to  cause  the  center  of 
illumination  to  be  shifted  slightly  above  the  plane  of  the  ecliptic 
in  March  and  slightly  below  this  plane  in  September.  (The  effect 
of  the  decrease  in  latitude  of  the  returning  streams  will  have  a 
precisely  similar  tendency.)  In  general,  at  any  time  of  the  year, 


By  J.  M.  Schaeberle. 


95 


the  illumination  at  any  angular  distance  from  the  Sun  will  be 
greatest  near  a  plane  which  contains  the  radius-vector  of  the  Earth, 
and  which  is  perpendicular  to  the  orthographic  projection  of  the 
Sun's  axis. 

The  phenomenon  will  be  least  conspicuous  in  December  and 
June,  and  most  conspicuous  in  September  and  March.  It  will 
always  be  brightest  near  the  Sun,  and  gradually  diminish  in 
intensity  to  within  a  certain  distance  of  the  point  which  is 
180°  from  the  Sun,  where  theoretically  there  will  be  a  slight 
increase  in  the  luminosity.  These  conditions  are  in  agreement 
with  actual  observation. 

Now,  the  effect  of  the  perturbations  of  the  superior  planets  is 
always  such  that  the  latitude  of  a  normally  ejected  returning 
stream  will  be  less  than  that  of  the  same  outgoing  stream;  con- 
sequently, these  streams  will  be  more  conspicuous  to  an  observer 
in  a  smaller  heliocentric  latitude  than  the  outgoing  streams.  If 
lines  are  drawn  from  the  Earth  tangent  to  the  incoming  stream, 
these  lines  will  all  have  a  slightly  less  longitude  than  that  of 
the  Earth,  so  that  the  center  of  the  secondary  maximum  will 
always  be  west  of  the  point  which  is  180°  from  the  Sun,  if  the 
returning  stream  is  more  conspicuous  than  the  outgoing  one, 
since  lines  from  the  Earth  drawn  tangent  to  the  outgoing  stream 
will  always  lie  eas}  of  the  same  point.  The  greatest  extent  will 
be  in  longitude. 

To  show  how  this  theory  agrees  with  observation,  I  give  be- 
low a  resume  of  the  published/  results  of  the  most  noted 
observers  of  the  Gegenschein.  I  have  taken  the  mean  results 
for  two  series,  one  corresponding  to  the  months  when  the  Earth 
was  above  the  Sun's  equator,  the  other  when  it  was  below  this 
plane: 


QMS 

rt>  p  a 

o£ 

<T>  «-+ 

P| 

^ 

o 

Period. 

fla 

<*9  £' 

ii 

Etc 

*l 

2, 

Q 

Observers. 

Reference. 

MS 

0  0  S 

£•£<* 

&0 

p.a 

.| 

F 

Mar.  to  April 

4-1-J9 

—  1°.5 

— 

12 

!•    SCHMIDT  . 

Astr. 

Aug.  to  N  ov. 
Feb.  to  May. 

4-2  .1 

0.0 

4-0  .2 
-2.0 

+ 

33 
32 

j   SEARLE  & 

Nach.,No.l726. 

Aug.  to  Oct.. 

—0.2 

+0.2 

4- 

11 

f  WENDELL.  _ 

...Astr.  Nach., 

Nos.  2376-2441. 

Sept.toOct.  . 

4-2.8 

—0.7 

— 

4 

{•  BARNARD  ._ 

Astr.  Jour- 

1* eo.  to  Mar. 

-f-0  .1 

4-0  .8 

4- 

11 

1 

nal,    No.     168. 

96       A  Mechanical  Theory  of  the  Solar  Corona, 

While  the  individual  observations  on  any  given  day  are 
often  very  discordant,  the  above  mean  results  certainly  show  a 
remarkable  agreement  with  the  theory. 

When  one  considers  that  the  area  covered  by  the  Gegenschein 
is  often  as  much  as  20°  long  by  10°  or  1 5°  wide,  the  difficulty 
of  accurately  locating  the  center  of  such  a  faint  object,  the 
caution  with  which  apparently  confirmatory  evidence  should 
be  regarded,  can  be  better  understood. 

In  any  given  latitude  the  effect  of  differential  atmospheric 
absorption  of  light  will  always  have  a  tendency  to  apparently 
shift  the  center  of  illumination  towards  the  zenith  of  the  place. 
In  northern  latitudes  (greater  than  23°. 5)  the  apparent  dis- 
placement due  to  atmospheric  absorption  will  always  be  greater 
in  June  than  in  December,  and  about  the  same  in  March  and 
September. 

Since  there  appears  to  be  no  marked  parallax  for  the  Gegen- 
schein, and  since  the  absence  of  strong  solar  light  within  the 
Earth's  shadow  appears  to  have  no  sensible  effect  on  the  central 
portions  of  this  illumination,  it  follows  that  much  the  greater 
portion  of  the  matter  composing  the  streams  must  be  much 
farther  away  from  the  Earth  than  the  length  of  the  Earth's 
shadow. 

Further  observations,  and  a  much  more  extended  comparison 
between  theory  and  existing  observations,  are  of  course  neces- 
sary before  definite  conclusions  can  be  drawn.  In  a  general 
way,  however,  I  have,  as  it  appears  to  me,  conclusively  shown 
that  a  phenomenon  similar  in  form  and  position  to  the 
observed  Zodiacal  Light  and  Gegenschein  must  necessarily  be 
produced  by  ejected  particles  whose  orbits  have  a  major  axis 
greater  than  the  Earth's  radius- vector  and  whose  theoretical 
perihelion  is  near  the  Sun's  center. 

FORWARD  DRIFT  OF  THE  SOLAR  SURFACE. 

The  planetary  perturbations  in  longitude  will  always  be  such, 
that  while  the  eccentricity  of  the  orbits  of  some  of  the  particles 
will  be  increased  (even  to  the  extent  of  causing  a  retrograde 
motion),  by  far  the  greater  number,  especially  those  having 
small  latitudes,  will  become  less  eccentric,  so  that  the  resultant 
effect  is  to  cause  the  returning  masses  to  strike  the  Sun  with  a 


By  J.  M.  Schaeberle.  97 

greater  angular  velocity  than  that  of  the  Sun's  surface,  thus 
causing  an  actual  forward  drift  of  this  surface,  which  will  be 
greatest  in  the  Sun's  equatorial  regions,  in  agreement  with  ob- 
servation. (A  variation  in  the  angular  distance  of  the  Gegen- 
schein  from  the  Earth's  radius-vector  produced  is  also  a  function 
of  the  planetary  perturbations  in  longitude.) 

TERRESTRIAL  MAGNETISM. 

We  know  from  actual  observation  that  the  atmosphere  of  our 
planet  is  continually  bombarded  by  meteoric  matter,  which  is 
often  volatilized  before  it  reaches  the  Earth's  surface.  If  we 
imagine  the  Earth  to  be  in  the  center  of  a  stream  of  uniformly 
distributed  matter  having  a  rectilinear  motion  in  a  given  direc- 
tion, it  is  at  once  evident  that  owing  to  the  rotation  of  the  Earth 
the  maximum  amount  of  meteoric  matter  will  fall  at  the  place 
which  has  the  least  linear  velocity  for  a  given  inclination  of 
the  local  horizon  to  the  direction  of  the  stream's  motion,  so  that 
at  the  equator  the  amount  of  matter  per  unit  of  the  area  will 
be  at  a  minimum,  while  a  very  decided  maximum  will  be  at 
each  pole.  Even  for  the  case  when  the  path  of  the  stream  is 
parallel  to  the  Earth's  equator,  the  area  about  the  poles  will,  on 
account  of  the  Earth's  mass,  still  receive  more  foreign  matter 
than  a  corresponding  area  nearer  the  equator,  since  particles 
will  not  only  be  deflected  from  the  more  distant  portions  of  the 
stream  so  as  to  strike  the  areas  near  the  poles,  but  the  new  instan- 
taneous orbits  described  by  these  more  distant  particles  will  be 
such  that  even  the  region  beyond  the  poles  will  be  bombarded. 
If  either  pole  is  inclined  towards  the  direction  from  which  the 
stream  is  coming,  the  amount  of  matter  received  at  that  pole 
will  be  enormously  greater  than  it  will  for  a  corresponding  area 
at  the  equator.  If  the  surface  on  which  the  matter  falls  is  per- 
manent, there  will  be  a  continual  accumulation  of  such  matter; 
if,  on  the  other  hand,  the  surface  is  a  movable  one,  like  water 
or  a  moving  field  of  ice,  the  matter  does  not  necessarily  accu- 
mulate at  the  place,  since  ocean  currents,  sooner  or  later,  will 
cause  a  general  distribution  over  the  globe. 

Now,  if  we  look  at  a  map  of  the  Earth,  we  find  that,  beyond  a 
certain  distance,  the  north  pole  is  almost  completely  surrounded 
by  land;  the  Arctic  Ocean  bounds  the  northern  coast  of  Europe, 
7 


98        A  Mechanical  Theory  of  the  Solar  Corona, 

Asia,  and  Alaska.  But  from  Eastern  British  America  towards 
the  pole  the  whole  area  is  practically  land-locked,  so  that  this 
area  will  contain  the  greatest  amount  of  accumulated  meteoric 
matter.  The  most  northerly  portions  of  Siberia  will  come  next 
in  order.  At  the  south  pole  practically  the  whole  Antarctic 
region  is  still  unexplored;  but  while  the  areas  of  maximum 
amount  of  accumulated  matter  cannot  be  accurately  located,  it 
is  at  once  evident  that  the  total  area  over  which  the  mass  of 
meteoric  matter  can  accumulate  will  be  much  greater  in  the 
Northern  than  in  the  Southern  Hemisphere. 

Now,  the  larger  meteoric  masses  which  reach  the  Earth's  sur- 
face are  found,  on  examination,  to  be  strongly  magnetic,  and 
the  smaller  masses  are  undoubtedly  magnetic  also.  Hence,  the 
arrangement  of  individual  meteoric  particles  covering  a  given 
surface  will  be  such  that  each  one  naturally  assumes  a  fixed 
position  with  reference  to  the  resultant  lines  of  magnetic  force. 
Of  the  two  poles  formed,  the  one  in  the  Antarctic  region  will 
(in  agreement  with  observation)  show  the  greatest  force,  since 
the  space  into  which  the  lines  of  force  are  condensed  will  be 
least  in  the  Southern  Hemisphere.  As  is  also  well  known  from 
actual  observation,  there  are  two  areas  or  centers  of  maximum 
force  near  each  magnetic  pole;  at  least  such  is  the  case  for  the 
Northern  Hemisphere,  where  the  area  of  greater  maximum  of 
force  is  in  Northern  British  America,  while  the  lesser  maximum 
is  in  Northern  Siberia.  A  possible  shifting  of  the  immense  ice 
fields  at  botn  poles,  of  course  involves  a  corresponding  move- 
ment of  the  meteoric  matter  imbedded  in  these  fields,  and  a 
consequent  shifting  of  the  centers  of  force  results.  The  direc- 
tion of  the  Earth's  magnetic  lines  of  force  should,  according 
to  this  theory,  be  largely  influenced  by  the  size,  outlines,  and 
locations  of  the  continents  of  the  globe;  and  a  summary  inspec- 
tion of  a  magnetic  chart  of  the  globe  indicates  that  such  is 
actually  the  case. 

THE  AURORA. 

Let  us  now  consider  the  phenomena  produced  by  the  passage 
of  the  Earth  through  a  particular  one  of  the  streams  ejected 
from  the  Sun.  In  certain  longitudes,  at  a  given  instant  of  time, 
the  direction  of  the  stream  will  be  more  nearly  at  right  angles 
to  the  direction  of  the  Earth's  magnetic  lines  of  force  than  in 


By  J.  M.  Schaeberle.  99 


other  longitudes.  Now,  in  the  case  of  a  permanent  magnet, 
wound  by  a  coil  of  some  conducting  material  in  the  form  of  an 
insulated  wire,  an  electric  discharge  can  be  produced  between 
the  terminal  points  of  this  wire,  if  a  magnetic  body  is  moved 
rapidly  across  the  lines  of  force  of  the  magnet;  the  discharge 
will  take  place  along  the  line  of  least  resistance.  Applying  this 
principle  to  the  case  of  the  Earth  and  the  stream,  then,  if  my 
reasoning  is  sound,  it  would  seem  to  follow  (1)  that  there  will 
be  a  tendency  for  a  discharge  to  take  place  between  the  particles 
of  the  stream,  and  that  (2)  such  a  discharge  will  be  in  the  direc- 
tion of  the  Earth's  magnetic  meridian;  since  each  individual 
particle  of  the  stream,  on  entering  the  Earth's  magnetic  field,  will 
at  once  take  such  a  position  that  the  line  joining  its  own  poles 
will  lie  in  the  direction  of  the  magnetic  meridian,  and  as  these 
same  particles  will  act  as  conductors,  the  lines  of  least  resist- 
ance will  be  formed  in  the  magnetic  meridians. 

If  we  take  it  for  granted  that  there  is  an  electrostatic  condi- 
tion in  which  a  positively  electrified  stratum  is  separated  from 
one  negatively  electrified  by  an  insulating  stratum  of  air,  then 
a  much  simpler  explanation  results.  The  lines  of  least  resist- 
ance will  be  formed  precisely  as  in  the  first  hypothesis;  these  lines 
joining  two  differently  charged  strata  will  evidently  be  shortest 
(and  the  discharges  therefore  most  brilliant)  at  the  magnetic 
poles,  while  near  the  equator  no  discharges  can  take  place,  since 
any  given  line  of  least  resistance  will  lie  wholly  within  a  given 
stratum.  The  intensity  of  the  discharge  will  decrease  as  the 
area  over  which  the  discharges  take  place  increases.  When 
the  number  of  discharges  is  very  great,  we  have  the  condition 
of  a  great  number  of  nearly  parallel  luminous  lines  more  or 
less  inclined  to  each  other,  so  that  in  addition  to  the  apparent 
motions  towards  the  magnetic  zenith,  concentric  arches  (rays) 
may  be  formed,  which  will  slowly  vary  with  variations  in  the 
arrangement  of  the  luminous  discharges.  (See  Plate  VIII., 
Figures  10  and  11,  inverted.  The  parallactic  effect  will  depend 
on  the  distance  of  the  display  from  the  observer,  so  that  the 
arches  (rays)  formed  may  be  either  convex  or  concave  in  per- 
spective.) Many  of  the  rapid  motions  may  be  only  apparent, 
and  due  to  an  actual  shifting  of  the  points  of  perspective 
intersection  of  continuous  discharges,  which  have  a  slight 
lateral  motion.  Figure  1,  Plate  VII.,  illustrates  the  low  auroral 


100      A  Mechanical  Theory  of  the  Solar  Corona, 


arch.  If  the  gratings  are  slightly  shifted,  this  luminous  arch 
can  be  changed  to  a  dark  segment.  Dark  segments  at  other  alti- 
tudes are  illustrated  in  Figures  10,  11,  12,  and  13. 

Gravitational  and  atmospheric  disturbances  will  constantly 
tend  to  break  existing  conductors,  and  to  form  new  ones  so  long 
as  the  suspended  particles  are  sufficiently  numerous. 

To  further  test  this  theory,  the  following  conditions  should 
be  fulfilled: 

As  the  streams  ejected  from  the  Sun  have  the  greatest  density 
in  about  15°  heliocentric  latitude,  the  number  of  auroras 
should  be  greatest  in  the  months  corresponding  to  the  times 
when  the  heliocentric  latitude  ft  of  the  Earth  is  greatest,  and 
least  when  latitude  of  the  Earth  is  zero.  As,  however,  a  return- 
ing stream  is  more  likely  to  pass  near  the  Earth  than  an  out- 
going one  (on  account  of  the  tendency  of  the  outer  planets  to 
diminish  the  latitudes  of  all  the  streams),  the  pole  which  is 
turned  towards  a  returning  stream  when  the  Earth  is  in  the 
plane  of  the  Sun's  equator  will  have  more  decided  displays 
than  the  one  turned  towards  the  Sun.  The  Earth  is  in  the 
plane  of  the  Sun's  equator  in  June  and  December,  and  during 
the  latter  month  the  north  pole  attains  its  greatest  inclination 
away  from  the  Sun,  so  that  the  frequency  of  auroras  should  be 
more  decided  in  the  Northern  Hemisphere  in  December  than  in 
June;  the  effect  of  the  longer  nights  will  also  cause  an  apparently 
greater  number  of  displays  in  December.  The  Earth  attains  its 
greatest  heliocentric  latitudes  in  March  and  September,  and  both 
poles  are  equally  exposed  to  the  solar  influences  at  these  times, 
consequently  the  auroras  should  not  only  be  most  numerous  at 
these  times,  but  in  both  months  the  number  should  be  about 
the  same.  I  take  the  following  data  from  the  article  on  Meteor- 
ology, Vol.  XVI.  of  the  Encyclopedia  Britannica: 
MONTHLY  FREQUENCY  OF  EUROPEAN  AURORAS. 


Jan. 

Feb. 

Mar. 

April. 

May. 

June. 

July. 

Aug. 

Sept. 

Oct. 

Nov. 

Dec. 

229 

307 

440 

312 

184 

65 

87 

217 

405 

497 

285 

225 

If  a  series  of  observations  should  be  manufactured  to  fit  this 
theory,  the  above  figures  could  hardly  be  improved  upon. 


By  J.  M.  Schaeberle.  101 


I  have  not  been  able  to  find  a  series  of  observations  for  the 
Southern  Hemisphere.  It  at  once  follows  that  if  the  streams 
have  periods  of  maxima  and  minima  of  magnitude  and  fre- 
quency, the  auroras  will  have  similar  and  nearly  coincident 
periods,  the  returning  streams,  as  a  rule,  governing  the  magni- 
tude of  the  display;  although,  when  the  perturbations  of  the 
streams  near  the  Sun's  surface  are  greatest,  the  slightly  deflected 
outgoing  streams,  from  the  higher  latitudes,  will  be  more  apt  to 
cross  the  Earth's  path.  If  these  streams  are  composed  of  small 
particles,  the  auroral  phenomena  will  be  largely  confined  to  the 
higher  regions  of  the  Earth's  atmosphere.  (So  far  as  the  final 
precipitation  of  such  particles  to  the  Earth  is  concerned,  the 
prevailing  direction  of  the  upper  atmospheric  currents  will  have 
much  to  do  with  the  final  location  of  such  masses  on  the  Earth's 
surface,  and  here,  again,  the  tendency  will  be  to  carry  these 
masses  towards  the  poles,  if  our  present  views  on  the  currents 
of  the  upper  atmosphere  are  correct.) 

The  monthly  variation  in  auroral  frequency  is  thus  accounted 
for.  The  variation  in  the  absolute  numbers  of  the  auroras,  tak- 
ing the  whole  world  together,  will  depend  upon  the  number  of 
the  streams,  and  will,  therefore,  pass  through  a  cycle  every  ten 
or  eleven  years,  precisely  as  the  Sun  spots  do,  according  to  the 
theory,  and  in  fact. 

VARIABLE  AND  NEBULOUS  STARS. 

It  seems  to  me  that  many  of  the  irregular  variations  in  the 
physical  appearances  of  certain  classes  of  stars  can  be  satis- 
factorily explained  by  the  theory  of  ejected  streams  colliding 
at  certain  intervals  with  the  returning  ones.  Viewed  from 
great  distances  such  stars  would  appear  to  be  surrounded  by 
nebulous  envelopes  of  varying  brightness,  and  according  to  the 
position  of  the  axis  of  rotation  and  the  zones  of  maximum 
activity  with  reference  to  the  line  of  sight  the  nebulosity 
would  appear  to  be  either  circular  or  more  or  less  elliptical  in 
outline.  The  bearing  of  this  theory  on  Professor  LOCKYER'S 
Meteoritic  Hypothesis  is  significant  (so  far  as  I  can  learn  from 
mere  notices  of  his  work  just  issued),  since  these  results  have 
been  obtained  without  any  preconceived  notions  as  to  whether 
the  explanation  of  certain  phenomena  would  agree  or  disagree 
with  any  other  theory. 


102      A  Mechanical  Theory  of  the  Solar  Corona. 


COMETS. 

The  hypothesis,  favored  by  some  astronomers,  that  the  matter 
now  revolving  about  the  Sun,  in  cometary  orbits,  was  once 
ejected  from  the  Sun,  is,  according  to  the  Mechanical  Theory, 
rendered  extremely  probable,  and  it  would  not  be  difficult  to 
bring  forward  many  strong  arguments  to  support  this  view  and 
to  account  for  many  apparent  changes  of  form  in  cometary 
matter.  But  the  length  of  this  postscript  has  already  far 
exceeded  my  original  intentions,  and  I  now  await  the  result  of 
the  final  verdict  as  to  the  merits  of  my  investigations,  to  be 
given  by  those  who  are  most  competent  to  pass  judgment. 


JKrtk 


fait- 


Yfest- 


JQiajframs  of  Zfc  flttinic. Intensity  oflkt 
Comas  of-  Wnaarw  <uul 
y  ££ 


Report  of  E.  E.  Barnard.  103 


IV.    REPORT  ON  THE  STANDARDIZING  OF  THE 
ECLIPSE  PLATES. 

By  E.  E.  BARNARD. 


The  plates  used  at  the  solar  eclipse  of  December  22,  1889,  by 
the  Lick  Observatory  party,  were  standardized  by  me  on  Sep- 
tember 24, 1889.  The  set  of  test-plates  designated  A,  B, J. 

were  also  standardized  at  the  same  time.  These  plates  were 
specially  ordered  from  the  SEED  Dry  Plate  Company  of  St.  Louis, 
in  August,  1889.  They  were  all  of  the  sensitometer  mark  26. 
The  eclipse  plates  of  January  1,  1889,  were  from  the  same 
makers,  and  also  have  the  sensitometer  mark  No.  26,  but  were 
not  specially  ordered,  being  bought  in  open  market.  The 
method  by  which  the  present  plates  were  standardized  was  the 
same  as  that  described  in  the  Report  of  the  January  Eclipse 
(p.  62).  The  programme  followed  for  the  present  (December 
22)  eclipse  is  given  by  Professor  HOLDEN  in  the  introduction  to 
this  report. 

Two  of  Mr.  BURNHAM'S  plates  (Nos.  1  and  4)  and  two  of  Mr. 
SCHAEBERLE'S  (Nos.  1  and  2)  received  squares  of  5,  10,  15,  20, 
30,  40,  50,  60,  70,  80  seconds  exposure.  The  ten  test-plates 

A,  B, j'also  received  the  same  number  of  squares  of  the 

above  exposure  times. 

Plates  A  and  B  were  taken  to  Cayenne,  and  developed  there 
by  Mr.  BURNHAM  on  December  24,  1889. 

Plates  C  and  D  were  taken  to  Cayenne,  and  returned  to  the 
Lick  Observatory  on  March  5, 1890.  They  were  restandardized 
on  March  sixteenth,  and  developed  (together  with  Plates  G  and 
H)  on  March  seventeenth;  all  four  being  placed  in  the  develop- 
ing tray  together  and  allowed  to  remain  exactly  the  same  length 
of  time.  The  standard  lamp  on  March  sixteenth  was  as  nearly 
as  possible  in  the  same  condition  as  on  September  twenty- 
fourth.  The  utmost  precaution  being  taken  to  conform  with 
the  programme  followed  in  its  treatment  on  the  date  of  the  first 
standardizing. 


104  Solar  Eclipse  of  December,  1889. 

Plates  E  and  F  remained  at  the  Lick  Observatory,  and  were 
developed  by  me  on  December  22,  1889. 

Plates  G  and  H  were  restandardized  March  sixteenth,  and 
developed  (with  C  and  D)  on  March  17,  1890. 

Plates  I  and  J  were  developed  immediately  after  they  were 
exposed  to  the  standard  lamp,  September  24,  1889. 

All  the  plates  which  went  to  Cayenne  were  carefully  wrapped 
in  their  original  boxes,  and  sealed  up  in  heavy  yellow  paper. 
The  plates  which  remained  at  the  Lick  Observatory  were  also 
in  their  original  boxes. 

Upon  the  return  of  the  eclipse  negatives,  the  different  por- 
tions of  the  corona  were  compared  by  me  with  the  standard 
squares  impressed  upon  the  same  plate.  From  the  comparisons 
of  the  standard  squares  on  Mr.  BURNHAM'S  plate,  No.  4,  I  have 
deduced  the  following  mean  values  for  the  apparent  density 
of  the  corona: 

FIRST  QUADRANT  (N.E.). 

A'=18'.2  (4  obs. )  a=l(y.8  (6  obs. ) 

6  =6. 0(5  obs.)  c=4.7(3  obs.) 

d=3'.2  (5  obs.) 

'SECOND  QUADRANT  (S.E.). 

A=13'.2  (3  obs. )  a=l(y.O  (4  obs. ) 

b  =  6  .4  (4  obs.)  c=  4  .0  (4  obs.) 

d=B'A  (4  obs.) 

THIRD  QUADRANT  (S.W.). 

A^=13.'4(4obs.)  a=l(y.7(6obs.) 

6=5.  3  (3  obs.)  c=  5. 2  (6  obs.) 

d=5M  (4  obs.) 

FOURTH  QUADRANT. 

AT=16'.9  (5  obs. )  a=ll'.2  (4  obs. ) 

b  =7. 3  (5  obs.)  c=  5. 7  (3  obs.) 

rf=5'.3(3obs.) 

And  for  the  entire  circuit  of  the  corona: 

A'=15'.42  (16  obs.)  «=l(y.68  (17  obs.) 

b  =  6  .25  (16  obs.)  c=  4  .90  (16  obs.) 

d=4'.25(16obs.) 

The  above  squares,  which  I  have  identified  as  K,  a,  6,  c,  d, 
received  the  following  durations  of  exposure  to  the  standard 

lamp: 

A"=10  seconds, 
a  =20  seconds. 
b  =40  seconds. 
c  =60  seconds. 
d  =70  seconds. 

In  the  above  comparisons  the  values  given  in  minutes  of  arc 
are  the  distances  from  the  Moon's  limb,  where  the  density  of 


Report  of  E.  E.  Barnard.  105 


the  corona  matched  that  of  the  different  squares.  For  instance, 
K==18'.2,  in  the  first  "quadrant,  means  that  from  all  the  com- 
parisons made  in  that  particular  quadrant  with  the  square  X, 
the  mean  gave  an  equal  density  of  the  corona  at  18'.2  from  the 
limb  of  the  Moon. 

The  method  by  which  these  comparisons  were  made  is 
explained  in  the  Report  of  the  Eclipse  of  January  1, 1889,  p.  63. 
From  the  observations  given  above  I  have  constructed  the  dia- 
gram shown  in  Plate  IX.,  to  which  has  been  added  a  similar 
diagram  for  the  eclipse,  of  January,  1889. 

E.  E.  BARNARD. 
LICK  OBSERVATORY,  September,  1890. 


OBSERVATIONS 


OF   THE 


LUNAR  ECLIPSE  OF  JULY  22,  1888, 


MADE   AT 


THE  LICK  OBSERVATORY. 


The  Lunar  Eclipse  of  July  22, 1888,  occurred  before  the  Lick 
Observatory  was  in  complete  working  order,  but  it  was  observed 
as  thoroughly  as  was  possible  under  the  circumstances. 

Some  of  the  results  obtained  appear  to  be  of  permanent  value, 
and  I  have  therefore  collected  the  work  of  the  various  observers 
into  one  whole,  and  beg  to  submit  it  as  the  first  contribution 
from  the  Observatory  which  JAMES  LICK  founded  in  1875. 

EDWARD  S.  HOLDEN.  • 
MT.  HAMILTON,  August  1,  1888. 


OBSERVATIONS  WITH  THE  36-INCH  TELESCOPE. 

Bv  EDWARD  S.  HOLDEN  and  J.  M.  SCHAEBERLE. 


The  visual  objective  of  the  great  telescope  was  used  to  form 
an  unenlarged  image  of  the  Moon  (6.51  inches  in  diameter,  or 
more  exactly,  6. 505 ±0.009,  as  measured  from  nineteen  draw- 
ings), projected  upon  sheets  of  white  cardboard  which  had  been 
previously  prepared. 

These  cards  were  laid  flat  upon  a  drawing  board,  at  right 
angles  to  the  optical  axis  in  the  principal  focus,  and  at  least 
three  points  of  the  circumference  of  the  Moon  were  marked 
upon  each  drawing.  In  order  to  orient  the  drawings,  the  out- 
line of  Mare  Crisium  was  drawn  upon  each  sketch,  until  10h  3m, 
Pacific  standard  time,  and  after  that  instant  the  positions  were 
fixed  by  marking  the  north  point  of  the  Moon  at  each  observa- 
tion. 

The  observation  itself  consisted  in  tracing  out  with  a  pencil 
the  outlines  of  the  various  shades  of  light,  and  marking  them 
darkest,  very  darJg,  dark,  pretty  bright,  bright,  brightest,  or  full 
sunlight,  according  to  circumstances.  These  terms  do  not  refer 
to  an  absolute  and  unvarying  scale  of  brilliancy,  but  must,  in 
strictness,  be  taken  on  a  new  scale  for  each  new  drawing. 
Practically,  however,  the  scale  is  constant  over  several  draw- 
ings. Forty-seven  such  drawings  were  made  at  the  telescope 
by  Mr.  SCHAEBERLE.  The  various  adjustments  of  the  clock  and 
instrument,  and  the  recording  of  the  times,  etc.,  were  done  by 
Professor  HOLDEN,  who,  in  the  intervals,  made  a  number  of 
naked-eye  sketches  of  the  eclipsed  Moon,  which  are  spoken  of 
in  another  section. 

The  times  were  recorded  by  means  of  chronometer  1,667,  whose 
corrections  to  Pacific  standard  time  were: 

At   8h  4««  of  its  face  — 2™  488.2 
At  12   8    of  its  face  —2    47  .0 

The  correction  — 2m  48s  has  been  used  throughout. 
The  observations  of  the  central  contacts  were: 


110  Lunar  Eclipse  of  July  22,  1888. 

gh  52m    6s,  P.  S.  T.,  the  intense  light;  ends. 
8   52    56,   P.  S.  T.,  totality  begins. 
*10    36    52,   P.  S.  T.,  totality  ends. 
1   43    56,  duration  of  total  phase. 

The  different  drawings  have  been  transferred  from  the  card- 
board sheets  (Moon's  diameter,  6.51  inches)  to  enlarged  photo- 
graphic prints  on  plain  paper  (about  5.7  inches  in  diameter). 
These  enlargements  were  made  from  a  negative  of  the  Moon 
(1.6  inches  in  diameter),  which  was  taken  by  Mr.  BARNARD 
with  the  12-inch  equatorial  immediately  after  the  end  of  totality. 
The  position  of  all  the  lights  and  shades  are  thus  correctly  kept 
in  the  copies. 

In  order  to  justly  estimate  the  value  of  these  drawings,  it 
should  be  kept  in  mind  that  the  illumination  of  the  whole  card- 
board was  sufficient  to  enable  the  various  lines  of  demarkation 
between  the  different  shades  to  be  distinctly  seen;  and  that  it 
was  not  sufficient  in  general  to  enable  the  observer  to  see  the 
pencil  line  which  he  had  just  drawn.  Hence,  each  line  drawn 
is  entirely  independent  of  all  the  others. 

Nothing  was  recorded  on  the  original  sketches  of  which  the 
observer  was  not  sure  at  the  time,  and  the  drawings  as  here 
given  are  accurate  copies  of  the  originals  on  a  slightly  reduced 
scale.  The  words  "  Dark,"  "  Very  Dark,"  etc.,  written  upon 
these  copies,  are  placed  exactly  where  the  observer  wrote  them 
upon  the  originals.  The  word  "Darkest"  has,  however,  been 
supplied  in  two  or  three  instances  where  notes  were  omitted  by 
the  observer.  D  stands  for  dark;  VD  for  very  dark;  HD  for 
half  dark;  B  for  bright;  VB  for  very  bright;  F  for  faint;  VF 
for  very  faint;  EF  for  extremely  faint. 

The  drawings  made  with  the  great  telescope  are  given  in  Fig- 
ures 1  to  42,  Plate  A.  They  serve  to  present  a  complete  account 
of  the  changes  of  light  and  shade  at  this  eclipse.  Unfortu- 
nately, some  of  the  copies  of  this  plate  are  not  satisfactory. 

Besides  the  drawings  here  given  certain  others  were  made,  as 
follows: 

One  at  8h  48m ;  omitted,  because  no  determining  point  was  marked  on  the  sketch, 
which,  therefore,  cannot  be  accurately  oriented. 

*  Possibly  the  image  of  the  Moon  may  not  have  been  well  centered  at  this 
time,  and  the  edge  of  the  corresponding  drawing  may  have  been  the  limit  of 
the  field  of  view,  which  would  have  made  the  contact  late.  (J.  M.  S.)  Mr. 
BARNARD'S  times  for  the  two  contacts  are  8h  53™  and  1011  36im. 


PLATE  A. 


DIAGRAMS  TO  ILLUSTRATE  THE  DISTRIBUTION  OF  LIGHT  AT  THE  LUNAR 
ECLIPSE  OF  JULY,   1 888,  BY  J.   M.  SCHAEBERLE. 


Report  of  Messrs,  ff olden  and  Schaeberle.       Ill 


One  between  8h  48m  and  8h  55m;  omitted,  because  no  determining  point  was 
marked  on  the  sketch,  which,  therefore,  cannot  be  accurately  oriented. 

One  at  8h  55m;  omitted,  because  no  determining  point  was  marked  on  the 
sketch,  which,  therefore,  cannot  be  accurately  oriented. 

One  at  8h  58m;  omitted,  because  no  determining  point  was  marked  on  the 
sketch,  which,  therefore,  cannot  be  accurately  oriented. 

One  at  ??;  omitted;  time  uncertain. 

One  at  9h  53m ;  omitted,  because  it  could  not  be  oriented. 

10h  33™  \  owttted,  because  both  were  drawn  on  the  same  side  of  the  paper. 
One  at  llh  13m;  omitted,  because  the  drawing  was  probably  not  well  centered. 
One  at  llh  40m ;  omitted,  because  it  is  simply  a  sketch  of  the  full  Moon  after 

the  eclipse,  drawn  for  the  purpose  of  identifying  the  various  features.    Its 

place  is  taken  by  the  enlarged  photograph,  Figure  1. 

The  notes  on  each  drawing  follow  immediately. 
NOTES  (See  PLATE  A). 

Figure    1.  General  view  of  the  uneclipsed  Moon. 

2.  9b    2m,  P.  S..T. 

3.  9h    3m. 

4.  9h    5m. 

5.  9t    8m. 

6.  9*  llm. 

7.  9h  13m.    The  border  of  the  Moon  was  not  marked  on  the  origi- 

nal, and  hence  the  outlines  are  somewhat  uncertain. 

8.  9h  15m. 

9.  9*  21m. 

10.  9h  23m. 

11.  9b  28m.    At  9h  27m,  the  circumference  can  be  seen  all  around.    A 

sudden  transition. 

12.  9h  31™. 

13.  9&  35™. 

14.  9h  44™. 

15.  9*  46™. 

16.  9h  51m. 

17.  9h  58">. 

18.  10h    2^. 

19.  10h    4m. 

20.  10h    6m. 

21.  10h    9m.    At  10h  7m,  the  S.  E.  commences  to  be  brighter. 

22.  10h  12m. 

23.  10h  13m.    The  borders  of  the  Moon  were  not  marked  on  the  origi- 

nal, and  they  are  therefore  somewhat  uncertain. 

24.  10h  17m. 

25.  10h  21m. 

26.  10h  22m. 

27.  10h  25m. 

28.  10h  27m. 

29.  10h  34m. 

30.  10h  36m.    Contact,  10h  36m  52s.     Possibly  the  image  may  not  have 

been  well  centered,  and  the  limit  of  the  field  of  view 
may  have  been  the  edge  of  the  drawing,  and  the 
contact  too  late  on  that  account. 


112  Lunar  Eclipse  of  July  22,  1888. 

Figure  31.  10h  41m.    There  is  a  narrow  border  of  penumbra  to  the  full  sun- 
light. 

32.  10h  45™. 

33.  1011  47m. 

34.  10*  49™. 

35.  1011  51«». 

36.  1Gb  53m. 

37.  llh    ()«». 

38.  l^    6". 

39.  llh  12™. 

40.  11*  17m. 

41.  llh  27m. 

42.  lit  3im. 

43.  Omitted. 

CONCLUSIONS  TO  BE  DRAWN  FROM  THE  OBSERVATIONS  WITH  THE 
GREAT  TELESCOPE. 

This  series  of  drawings,  together  with  the  naked-eye  draw- 
ings, shows,  in  a  systematic  and  thorough  manner,  a  fact  that 
has  frequently  been  previously  observed,  namely,  that  during 
a  lunar  eclipse  that  portion  of  the  interior  of  the  Earth's  shadow 
which  is  projected  on  the  lunar  disk,  from  time  to  time,  does  not 
appear  to  be  uniformly  illuminated. 

The  series  also  satisfactorily  shows  that  the  necessary  and 
sufficient  cause  of  these  variations  in  brilliancy  is  found  in  the 
different  reflective  powers  of  different  regions  of  the  Moon's  sur- 
face. It  appears  to  us  that  it  is  only  necessary  to  state  this 
conclusion  and  to  refer  to  the  drawings  for  its  proof.  If  this  be 
so,  such  changes  observed  at  future  lunar  eclipses  may  be  at 
once  referred  to  the  same  cause. 

We  may  point  out,  what  indeed  is  obvious,  that  these  observa^ 
tions  are  exactly  suited  to  be  the  basis  of  a  thoroughgoing  pho- 
tometry of  the  Moon's  surface,  and  that  it  may  be  well  to  observe 
a  few  more  lunar  eclipses  in  the  same  manner  for  the  sake  of 
comparison. 


Report  of  Edward  S.  H olden.  113 


NAKED-EYE  DRAWINGS. 

By  EDWARD  S.  HOLDEN. 


In  the  intervals  of  observation  with  the  large  telescope,  I 
made  eleven  sketches  with  the  naked  eye.  On  each  sketch  I 
marked  the  boundaries  of  the  regions  of  differing  color  or  shade. 
Mr.  KEELER  also  made  a  drawing  with  the  naked  eye. 

The  sketches  have  been  copied  carefully  onto  blue  prints 
from  a  negative  of  the  uneclipsed  Moon,  made  by  Mr.  BARNARD 
immediately  after  totality,  with  the  12-inch  equatorial. 

It  will  be  noticed  that  in  general  the  lines  of  demarkation 
referred  to  seem  to  follow  lines  of  topographic  or  photometric 
difference  on  the  Moon's  surface.  There  appear  to  be  few  excep- 
tions to  this,  and  it  seems  that  the  "wedge-shaped  "  shadow  and 
the  curious  interior  forms  observed  at  this  and  at  other  lunar 
eclipses  are  shown  by  these  naked-eye  drawings  alone  to  be 
caused  mainly  by  differences  of  reflecting  power  in  the  various 
parts  of  the  Moon's  surface. 

These  drawings  follow  Plate  B  (Figures -44  to  55).  Some  of 
the  copies  of  Plate  B  are  not  satisfactory. 

NOTES  (See  PLATE  B). 

Figure  44.  8h  26m.  P.  S.  T.  A=>dull  chocolate  red.  B=brighter  chocolate 
red.  C=full  moonlight.  The  arrangement  of  color, 
as  described,  was  first  noticed  at  8h  26m,  but  may  have 
existed  previously. 

45.     .    A=darker.    B=bright  chocolate  red,  inclining  to  cop- 

per color.   C=full  moonlight.   8h  53m,  totality  begins. 
Color,  a  dull  red. 

46.  8h  58m.    A=much  darker  than  the  rest  of  the  disk,  which  hardly 

looks  as  if  it  were  obscured. 

47.  9h    2m.    A=deep  copper  color.      B=yellow.      C=inclining  to 

copper  color. 

48.  9h  13m.    The  yellow  of  B  is  like  the  yellow  at  the  limb  of  Mars 

(lemon  yellow).    The  red  is  like  the  red  of  Mars,  only 
not  so  vivid.    The  shadow  (A)  is  wedge-shaped. 

49.  9h  17m.    A=dark.      B=lemon  yellow.      C=copper  color.      At 

9h  40m,  the  whole  disk  is  dark.    At  9h  45m,  middle  of 
eclipse. 

50.  10h    3m.    The  lemon  yellow  (B)  is  now  on  the  east  side. 


114  Lunar  Eclipse  of  Jiily  22,  1888. 


Figure  51.  1011  21m.    A=red.     B=lemon  yellow.     C=a  dark  square.     The 
shadow  (A)  is  wedge-shaped. 

52.  10h  29™.    A=coppery  red.    B=lemon  yellow.    B  separates  into 

two  parts  at  the  east  limb.  C=dark.  10h  37m  is  the 
end  of  totality. 

53.  — .    A— full  moonlight.    The  circle  of  the  terminator  of  the 

bright  Moon  appears  to  be  of  a  larger  radius  than 
the  circle  of  the  eclipsed  Moon,  and  so  remains  until 
11>  15m. 

54. .     A«=gray.     B=coppery  tinge.     C=full  moonlight. 

55.  — .  By  Mr.  KEELEK.  Appearance  shortly  after  III.  con- 

tact. 


PLATE  B 


NAKED  EYE  SKETCHES  OF  THE  LUNAR  ECLIPSE  OF  JULY,   1 888, 
BY  E.  S.  HOLDEN  AND  J.  E.   KEELER. 


Report  of  J.  E.  Keeler.  115 


SPECTROSCOPIC  OBSERVATIONS. 

By  J.  E.  KEELER. 


The  observations  which  I  made  during  the  total  lunar  eclipse 
of  July  twenty-second  were  for  the  purpose  of  ascertaining 
whether  any  unusual  phenomena  were  presented  by  the  spectra 
of  immersed  portions  of  the  Moon's  surface. 

A  small  direct-vision  spectroscope  by  BROWNING,  containing 
five  prisms,  was  used  with  the  12-inch  equatorial.  The  diame- 
ter of  the  emergent  beam  was  about  one  tenth  of  an  inch,  and 
hence  the  full  aperture  of  the  object  glass  was  utilized.  The  spec- 
troscope was  inserted  in  the  eyepiece  tube  of  the  micrometer 
belonging  to  the  telescope,  so  that  it  could  be  moved  across  the 
field  by  turning  the  pinion  of  the  eyepiece  slide,  and  the  posi- 
tion circle  of  the  micrometer  was  set  so  that  this  motion  was  in 
a  parallel  of  declination,  and  at  right  angles  to  the  direction  of 
the  spectroscope  slit. 

Before  totality  began,  the  telescope  was  directed  to  Jupiter, 
and  the  spectroscope  adjusted.  The  lines  in  the  spectrum  of 
the  planet  were  sharply  seen,  and  the  slit  was  opened  as  wide  as 
possible,  without  too  great  a  sacrifice  of  definition.  A  notch  was 
made  on  the  eyepiece  slide  to  mark  the  point  of  coincidence 
with  the  cross- wires  of  the  finder.  None  of  the  adjustments 
were  disturbed  during  the  eclipse. 

Turning  to  the  Moon,  which  had  just  completely  entered  the 
umbra,  a  continuous  spectrum  was  seen,  but  without  dark  lines, 
simply,  in  my  opinion,  because  the  brightness  was  insufficient. 

Mr.  HILL,  who  assisted  me  in  these  observations,  pointed  the 
telescope  by  means  of  the  finder,  and  we  went  over  the  surface 
of  the  Moon  many  times,  and  also  selected  portions  which 
seemed  in  any  way  remarkable,  but  nothing  was  seen  except  a 
continuous  spectrum,  narrowing  down  in  the  darker  regions 
to  a  mere  band  of  greenish  light.  The  point  of  maximum 
brightness  was  further  up  in  the  spectrum  than  I  should  have 
expected  from  the  color  of  the  eclipsed  Moon. 

At  about  10h  6m  we  placed  the  slit  on  Aristarchus,  which  was 
shining  brightly  in  the  deep  shadow,  and  the  bright  band  it 


116  Lunar  Eclipse  of  July  22,  1888. 

gave  in  the  general  spectrum  of  the  surface  was  quite  remarka- 
ble, the  yellow  shining  out  with  almost  star-like  brilliancy. 

Other  bright  points  were  also  observed,  but  showed  nothing 
but  a  brightening  of  the  continuous  spectrum. 

As  the  east  limb  of  the  Moon  began  to  brighten,  I  kept  the 
spectroscope  on  the  brightest  part,  and  first  saw  the  FRAUNHOFER 
lines  at  10h  33m.  Just  before  this  I  thought  I  could  catch  two 
faint  bright  lines,  one  just  below  the  yellow  and  one  in  the  green, 
but  further  watching  convinced  me  that  this  was  illusory,  and 
due  to  contrast  with  the  dark  lines  of  the  spectrum,  then  just 
beginning  to  appear.  With  so  low  a  dispersion,  the  yellow  of 
the  solar  spectrum  appears,  to  me  at  least,  almost  like  a  bright 
line,  partly  because  it  is  so  narrow,  and  the  brightness  reaches 
there  so  sharp  a  maximum,  and  partly  because  it  is  contrasted 
with  the  dark  shade  of  the  D  lines,  which  throws  it  into  relief. 

A  few  minutes  after  10h  33m  the  limb  of  the  Moon  under 
examination  emerged  from  the  umbra.  The  FRAUNHOFER  lines 
could  be  seen  just  within  the  boundary,  but  not  in  the  deep 
shadow. 

COLOR. 

The  color  near  the  edge  of  the  umbra,  when  the  Moon  was 
fully  eclipsed,  was  bright  orange,  shading  into  a  deep  copper 
red  toward  the  center  of  the  shadow,  where  it  was  a  dark 
dusky  red.  The  red  color  was  more  marked  than  in  any 
eclipse  I  have  seen.  As  the  Moon  passed  out  of  the  shadow, 
the  parts  which  brightened  first  were  not  always  those  nearest 
to  the  boundary  of  the  shadow,  but  examination  of  the  Moon 
after  the  eclipse  showed  that  these  were  always  portions  of 
superior  reflecting  power. 

While  the  shadow  was  passing  off,  Mr.  HILL  remarked  that 
the  inner  edge  of  the  umbra  was  marked  with  a  band  of  green- 
ish gray  tint,  shading  into  the  red.  This  band  was,  roughly, 
one  fourth  of  the  Moon's  diameter  in  width. 

Shortly  after  the  east  limb  of  the  Moon  emerged  from  the 
umbra  I  made  a  naked-eye  drawing,  which  is  given  in  Plate  B, 
Figure  55,  showing  a  broad  band  of  shade  extending  across  the 
still  eclipsed  portion  in  the  direction  of  the  Moon's  motion. 
This  effect  disappeared  in  the  finder. 

One  occultation  was  observed  with  the  finder,  but  the  power 
was  insufficient  to  enable  any  degree  of  accuracy  to  be  attained. 


Report  of  E.  E.  Barnard.  \\1 


OBSERVATIONS. 

By  E.  E.  BARNARD. 


The  total  eclipse  of  the  Moon,  July  twenty-second,  was 
observed  with  the  6^-inch  equatorial  and  photographed  with 
the  12-inch. 

The  evening  was  clear,  with  a  high  west  wind. 

When  the  Moon  was  first  seen  above  the  haze  and  clouds  in 
the  east,  it  was  perceptibly  tinged  with  penumbra.  A  low 
power,  giving  a  field  of  1-|°,  was  used  on  the  6^-inch,  with  a  view 
to  determine  the  extent  of  the  internal  illumination  of  the 
Earth's  shadow.  On  account  of  the  extremely  gradual  transi- 
tjxm  from  the  edge  of  the  umbra  to  the  more  strongly  illuminated 
interior  of  the  shadow,  it  was  found  impossible  to  determine 
with  any  trustworthiness  the  true  extent  of  this  phenomenon. 

The  observations  were  considerably  broken  by  the  time  taken 
to  get  the  photographing  arrangements  in  position  on  the  12- 
inch  before  and  after  totality,  as  the  instrument  was  used 
throughout  totality  by  Mr.  KEELER. 

I  have  thought  it  advisable  to  give  my  observations  in  full, 
as  they  were  carefully  made  and  may  prove  of  value  in  future 
eclipses.  I  shall,  therefore,  transcribe  from  my  notes  with  but 
a  few  changes  for  brevity's  sake. 

Unless  indicated  by  the  word  "  eye,"  the  observations  were 
made  with  the  6^-inch  telescope,  with  low  power  as  stated. 

At  7h  27m  the  penumbra  is  faintly  shading  the  north  following 
limb,  also  perceptible  to  the  eye. 

7h  33m;  smoky  at  n.  f.  limb,  perceptibly  deepening  to  the  eye. 

7h  35m;  smokiness  more  decided,  extending  over  one  third  the 
disk — no  definite  determination. 

7h  42m;  pretty  thick  and  smoky  at  n.  f.  limb,  and  extending 
gradually  over  one  half  of  the  disk.  To  eye,  it  is  decidedly 
smoky  at  lower  left-hand  limb — extending  at  least  over  one 
half  of  the  disk. 

7h  47m;  moderately  thick  smoky  shade,  with  faint  brownish 
tinge  at  limb. 


118  Lunar  Eclipse  of  July  22,  1888. 

7h  50m;  deepening  at  limb  and  seeing  improved.  There  is  no 
brownish  tinge  now — probably  the  preceding  record  is  due  to 
poor  seeing  and  low  altitude. 

7h  53m;  deeper  shade  at  n.  f.  limb. 

7h  54m;  shading  very  noticeable  to  eye. 

7h  55^m;  very  heavy  shade  touching  limb. 

7h  55|m;  unmistakably  the  true  shadow. 

7h  56m;  limb  fading  under  the  shadow.  To  eye,  a  decided 
blunting  of  the  lower  left-hand  edge,  as  if  flattened. 

7h  57-|m;  the  limb  immersed  to  a  depth  of  one  third  of  the 
distance  from  Copernicus  to  Aristarchus.  Up  to  this  time  no 
red  had  been  noticed  at  the  limb.  Ceased  observing  to  make 
some  exposures  with  the  12-inch  telescope. 

8h  9m;  with  the  3-inch  finder  of  the  12-inch,  the  limb  was 
noticed  to  be  decidedly  tinged  with  red.  Returning  to  the  64- 
inch,  the  observations  were  resumed. 

8h  48m;  the  edge  of  shadow  bisects  the  Mare  Crisium.  It  ;s 
impossible  to  decide  on  any  definite  termination  to  the  red 
shade  into  which  the  greater  part  of  Moon  is  immersed,  but  at 
this  time  the  edge  of  the  true  shadow  would  bisect  the  line  from 
the  bright  limb  to  the  estimated  termination  of  the  red. 

8h  50m;  the  red  shade  touches  the  foil,  edge  of  the  Mare 
Crisium,  and  deepens  to  the  foil,  limb  of  Moon. 

An  endeavor  was  made  to  observe  as  accurately  as  possible 
the  moment  of  immersion  of  the  p.  limb  in  the  shadow. 

8h  53m;  the  sunlight  disappears. 

8h  53|m;  certainly  wholly  within  the  shadow.  The  edge  of 
shadow  during  and  just  before  immersion  was  so  softly  diffused 
as  to  be  all  but  indeterminate,  but  the  time  of  disappearance 
was  quite  decided. 

8h  55m;  the  red  coloring  now  extends  to  the  middle  of  the 
Mare  Crisium]  there  is  no  decided  termination  to  it,  but  I  think 
it  would  not  be  detected  as  red  beyond  the  middle  of  this  Mare . 
The  red  coloring  is  by  no  means  so  clear  and  decided  as  at  the 
eclipse  of  June  11,  1881.  It  is  of  a  slight  reddish  brown — a 
very  poor  dull  color. 

•  8h  58m;  the  Moon  is  now  wholly  within  the  red;  the  f.  .half 
is  a  poor  but  heavy  red,  the  p.  half  a  lighter  red,  somewhat 
weakened  with  yellow.  The  red  is  dullish,  not  clear.  To  eye, 
the  Moon  is  dull,  the  lower  left-hand  edge  nearly  lost  from  dim- 


Report  of  E.  E.  Barnard.  119 

ness,  the  upper  right-hand  edge  gradually  brighter  and  of  an 
orange  color. 

9h  10m;  in  the  foil,  portion  the  details  hazy  and  faintish,  while 
those  of  the  preceding  are  clearer  and  brighter;  the  f.  portion 
a  poor  smoky  red  or  brownish,  and  the  preceding,  watery  red. 
With  eye,  the  east  limb  is  scarcely  discernible. 

9h  37m;  almost  uniformly  covered  with  dull,  smoky,  reddish- 
yellow  light;  the  p.  portion  brighter;  f.  side  poor  and  dullish; 
details  very  hard  to  make  out;  the  outline  of  Moon  clearly 
defined  against  the  sky;  Tycho  seen  with  difficulty. 

9h  30m;  the  f.  limb  is  perceptibly  brightening.  The  heavier 
obscuration  is  about  central,  and  covers  nearly  all  the  Moon; 
probably  heaviest  over  Tycho,  which  is  badly  blotted  out;  heavy 
also  to  the  north,  augmented  by  the  plains. 

9h  40m;  the  f.  limb  brightening;  the  great  dusky  mass,  extend- 
ing north  and  south  through  the  middle,  is  not  so  red.  To 
eye,  the  Moon  is  very  dull. 

9h  45m;  to  eye,  the  Moon  is  very  dull  and  dim,  and  of  a  dull, 
dirty,  coppery  tinge.  There  is  a  large,  dusky,  roundish  spot, 
symmetrical  with  the  center,  and  wTith  radius  equal  to  eight 
tenths  that  of  Moon.  The  Moon  is  no  more  conspicuous  than 
the  brighter  parts  of  the  Milky  Way.  I  was  struck  with  its 
dullness,  and  the*  utter  absence  of  any  illumination  of  the  sky 
from  it.  The  sky  was  black,  and  the  stars  everywhere  shone 
as  if  no  Moon  existed. 

9h  47-Jm;  the  n.  f.  limb  is  brightening  in  red  color,  while  the 
shade  is  passing  to  the  s.  preceding.  The  north  pole  is  also 
brightening. 

9h  53m;  to  eye,  the  lower  left-hand  limb  is  brightening;  the 
Moon  dim;  the  Milky  Way,  the  Andromeda  nebula,  the  cluster 
in  Perseus,  etc.,  as  bright  as  if  no  Moon  existed. 

9h  57m;  the  n.  f.  limb  brightening  rapidly,  Tycho  and  stream- 
ers coming  out  plainly.  The  color  of  the  Moon  is  a  mixture 
of  pale  yellow  and  pale  red,  with  a  dullness  of  smoke.  All 
the  s.  p.  portion  of  Moon  is  dusky,  with  little  warmth  of  color, 
and  no  transparency. 

10h  7m;  with  eye,  rapidly  brightening  on  lower  left-hand  edge; 
examined  with  a  high  power,  and  the  surface  comes  out  very 
poorly.  There  is  no  sharpness  of  detail;  it  appears  as  if  one 


120  Lunar  Eclipse  of  July  22,  1888. 

were  looking  through  a  confusing  dust  veil.  The  right-hand 
limb  is  scarcely  distinguishable  with  the  eye. 

I0h  28m;  the  entire  fol.  half  is  brightish  white;  the  p.  side  is 
a  dusky,  smoky-red  brown. 

10h  30m;  the  s.  f.  limb  very  red;  the  n.  p.  heavier  reddish 
brown. 

10h  35|m;  bright  at  limb— the  edge  of  shadow. 

10h  36^m;  contact  certainly  past;  the  south  pole,  and  all  about 
Tycho  a  beautiful  orange  yellow;  the  p.  portion  brownish  red. 

10h  40m;  the  line  of  red  would  probably  pass  through  Coper- 
nicus. The  entire  p.  portion  assuming  a  more  transparent 
appearance;  the  region  from  Copernicus  to  edge  of  Moon  a 
clear  gray  color;  the  p.  limb  very  heavy,  in  clear  reddish 
brown.  Shadow  pretty  well  defined. 

10h  44|m;  shadow  bisects  Aristarchus. 

.10h46im;  shadow  bisects  Kepler. 

10h  54m  ;  shadow  bisects  Tycho. 

10h  54  Jm;  shadow  bisects  Copernicus. 

The  line  of  shadow  swept  by  these  last  two  craters  almost  at 
same  instant,  but  Copernicus  was  certainly  a  fraction  of  a  min- 
ute later  than  Tycho.  These  last  observations  will  be  good,  as 
the  shadow  was  pretty  well  defined,  and  the  motion  rather  fast. 

Stopped  here  to  make  exposures  on  the  12-inch.  .Returned 
to  6^-inch. 

llh  34m;  the  shadow  very  pale  and  difficult  to  see;  it  is  now 
probably  at  the  limb. 

llh  36^m;  probable  contact,  but  very,  very  uncertain. 

llh  38m;  certainly  free  of  shadow,  but  still  a  faint  tinge  of 
shade.  The  portion  of  the  Moon  where  the  shadow  left  was 
scarcely  different  in  shade  from  the  shadow,  and  it  was  impos- 
sible to  be  certain  when  contact  occurred.  This  observation  is 
poor,  and  is  probably  late. 

The  sky  was  clear  throughout.  The  records  are  in  standard 
Pacific  time,  which  is  8h  slow  of  Greenwich. 

REMARKS. 

Compared  with  the  total  eclipse  of  June  11,  1881,  this  was  a 
much  less  splendid  phenomenon,  the  Moon  appearing  of  a 
smoky  reddish-brown  color,  and  the  details  during  totality 


Report  of  E.  E.  Barnard.  m 

singularly  indistinct.  As  a  naked-eye  spectacle  it  was  far  less 
striking  than  the  ^eclipse  of  1881.  During  the  middle  of  the 
eclipse  the  Moon  was  but  feebly  luminous  to  the  eye,  though 
quite  conspicuous.  It  appeared  of  a  smoky  brownish-red  color, 
being  no  more  conspicuous  than  the  brighter  parts  of  the  Milky 
Way;  the  stars  and  the  great  Andromeda  nebula  were  as  bright 
and  the  sky  as  dark  as  if  no  Moon  were  present.  There  was 
an  almost  total  absence  of  the  beautiful  transparent  red  color 
that  made  the  eclipse  of  1881  so  striking. 

In  this  eclipse  it  was  impossible  to  decide  as  to  the  exact 
extent  of  the  internal  illumination  of  the  shadow. 

During  the  latter  part  of  eclipse  the  shadow  seemed  to  become 
more  transparent,  probably  due  to  the  increasing  altitude  of 
the  Moon. 

Near  10h  30m  a  9^m  star  was  occulted,  and  before  disappear- 
ance appeared  to  be  projected  on  the  Moon  by  probably  its  / 
whole  diameter,  the  disappearance  being  at  the  n.  f.  limb,  which  V  I 
was  bright  with  its  approach  to  the  edge  of  the  shadow. 

Twelve  photographs  in  all  were  made — six  before  and  six 
after  totality. 


CONTACTS  WITH  SHADOW,  LUNAR  ECLIPSE  OF 
JULY  22,  1888. 

Observed  with  small  spy-glass,  by  C.  B.  HILL. 


I.  At  7h  54m  35s  by  watch,  or  at  7h  54m  09s  Pacific  standard 
time;    good  observation;  hesitated  nearly  10s  before  marking 
time. 

II.  At  8h  55m  10s  by  watch,  or  at  8h  54m  42s  Pacific  standard 
time;  difficult  observation;  "  probably  15s  late." 

III.  and  IV.  were  not  observed,  as  I  was  occupied  in  assist- 
ing Mr.  KEELER  in  his  spectroscopic  work. 


CATALOGUE  OF  THE  LIBRARY 


LICK   OBSEEVATOEY 


OF  THE 


UNIVERSITY  OF  CALIFORNIA. 


PART  I— TO  JULY  1,  1890, 


PREPARED  BY  EDWARD  S.  HOLDEN. 


PRINTED  BY  AUTHORITY  OF  THE  REGENTS  OF  THE  UNIVERSITY  OF  CALIFORNIA. 


SACRAMENTO: 

STATE   OFFICE,   :  :    A.    J.   JOHNSTON,    SUPT.    STATE  PRINTING. 

1891  . 


INTRODUCTORY  NOTE. 


The  books  in  the  library  have  come  from  the  following  sources: 
(a)  Books  purchased  by  the  Lick  Trustees  between  1875  and 
June  1,  1888,  mostly  on  the  recommendation  of  Professor  NEW- 
COME,  U.  S.  N.,  or  of  myself.  A  list  of  some  of  these  works  is 
printed  as  an  Appendix  to  the  Catalogue  of  the  Library  of  the 
American  Ephemeris,  Washington,  1883. 

(6)  Duplicate  books  transferred  from  the  General  Library  of 
the  University  of  California  by  order  of  the  Regents  (1887). 
(Duplicate  and  other  books  not  needed  in  the  work  of  the 
Observatory  are  regularly  turned  over  to  the  General  Library 
of  the  University  at  Berkeley;  but  all  the  more  important  series 
have  their  titles  printed  in  the  following  catalogue.) 

(c)  Books  purchased  by  the  Regents  of  the  University  since 
June  1,  1888. 

(d)  Books  presented  to  the  library  by  scientific  societies  and 
institutions,  by  men  of  science,  and  by  other  friends  of  the 
Observatory,  both  at  home  and  abroad.     I  have  transferred  to 
the  library  from  my  own  private  collection  a  very  great  number 
of  books  and  pamphlets  which  were  needed  for  use  in  the 
Observatory. 

(e)  Books  temporarily  loaned  to  the  Observatory  and  depos- 
ited in  its  collections. 

The  following  pages  contain  a  catalogue  of  the  books  and 
pamphlets  in  the  library  on  July  1,  1890.  The  catalogue  is 
strictly  alphabetical  by  authors,  with  the  following  exceptions: 

(1 )  The  title  word  for  an  observatory  or  for  a  scientific  society 
is  taken  to  be  the  city  in  which  the  observatory  or  society  has 
its  permanent  home,  as  Greenwich  (Royal  Observatory),  etc. 

(2)  The  title  word  for  scientific  journals  is  taken  to  be  the 
name  of  the  journal,  as  Astronomische  Nachrichten,  etc. 

(3)  The  title  word  for  the  Government  publications  of  each 
country  is  taken  to  be  the  name  of  the  capital  city  of  the 
country,  as  Washington  (U.  S.  Department  of  State). 

(4)  All  dictionaries  are  catalogued  together  under  the  word 
Dictionary,    and    all    encyclopaedias   are    catalogued   together 


4*  Catalogue  of  the 


under  Encyclopaedia,  and  cross-references  are  inserted  at  the 
names  of  the  authors. 

Framed  photographs  and  pictures  (only)  are  catalogued. 
These  are  displayed  in  the  various  rooms  of  the  Observatory 
building.  Unframed  and  unmounted  photographs,  etc.,  are 
preserved  in  the  library  drawer  "  Photographs,"  or  in  port- 
folios. 

Complete  volumes  published  by  an  observatory,  etc.,  are 
credited  to  the  institution;  extracts  from  observatory  publica- 
tions are  usually  credited  to  the  author  and  not  to  the  institu- 
tion. The  Greenwich  Star  Catalogues  are  indexed  under  AIRY 
and  CHRISTIE,  for  example.  Cross-references  are  introduced 
where  it  seems  to  be  necessary. 

There  are  no  subject  titles  in  this  catalogue,  except  for  diction- 
aries and  encyclopaedias  as  above.  Pamphlets,  or  unbound 
books,  are  here  catalogued  precisely  like  bound  works,  except 
that  they  are  distinguished  by  the  character  P  at  the  conclu- 
sion of  the  entry. 

The  format  of  books  here  set  down  relates  rather  to  their 
size  than  to  the  folding  of  their  leaves.  No  attempt  has  been 
made  to  distinguish  between  octavos  and  duodecimos,  for 
example,  when  their  pages  are  of  the  same  size.  For  exact 
bibliographic  information  of  the  kind,  reference  should  be  made 
to  the  catalogues  of  the  great  astronomical  library  at  Pulkowa, 
or  to  other  well  known  sources. 

It  should  be  mentioned  that  all  known  errata  (some  ten 
thousand  to  twelve  thousand  in  number)  in  our  Star  Cata- 
logues have  been  corrected  with  the  pen  up  to  the  beginning 
of  the  year  1886,  from  a  list  prepared  by  myself.  It  is  intended 
to  keep  up  this  practice. 

During  my  stay  at  Mount  Hamilton 'in  the  summer  of  1886, 
at  the  invitation  of  the  Lick  Trustees,  I  made  the  present  cata- 
logue complete  to  that  time.  On  account  of  the  great  conven- 
ience of  a  complete  catalogue,  and  as  there  was  no  other  person 
to  do  this  work,  I  have  taken  the  time  to  bring  the  catalogue 
up  to  July  1,  1890.  Messrs.  C.  B.  HILL  and  A.  J.  BURNHAM 
have  assisted  in  a  portion  of  the  cataloguing. 

One  word  may  be  said  as  to  the  arrangement  of  the  books 
and  pamphlets  in  the  library-room.  The  bound  books  are 
arranged  on  the  shelves  strictly  by  subjects,  and  the  shelves 
have  general  labels,  as  follows: 


Lick  Observatory  Library.  5* 


General  Astronomy.  Ephemerides. 

Star  Catalogues.  Publications  of  Scientific  Societies. 

Star  Maps  and  Atlases.  Smithsonian  Institution. 

Astronomical  and  Mathematical  Tables.  Scientific  Periodicals. 

Astronomische  Nachrichten.  Mathematics. 

Paris  Academy  of  Sciences.  Physics  and  Chemistry. 

United  States  Coast  and  Geodetic  Survey.  Bibliography. 

Royal  Society  of  London.  Meteorology. 

Publications  of  Observatories.  Miscellaneous. 

The  pamphlets  and  unbound  books  are  kept  in  large  drawers, 
a  drawer  being  (usually)  devoted  to  each  subject.  Periodicals 
are  preserved  in  open  pigeon  holes  and  in  racks. 

The  labels  of  the  drawers  are  as  follows: 

1.  Mathematics.  25.  Obliquity,   Precession,  Aberration, 

2.  Mathematical  Tables.  and  Nutation. 

3.  Cosmology,  Cosmography.  26.  Proper  Motions  and  Parallaxes  of 

4.  Spherical  Astronomy.  Fixed  Stars. 

5.  Theoretical  Astronomy.  27.  Reports  of  Observatories. 

6.  Theory  of  Instruments.  28.  Miscellaneous  Astronomical  Obser- 

7.  Chronology.  vations. 

8.  Catalogues  of  Stars.  29.  Mechanics,  Chemistry. 

9.  Ephemerides.  30.  Heat,  Sound,  and  Electricity. 

10.  Astronomical  Tables.  31.  Optics  and  Photometry. 

11.  Geodesy.  32.  Meteorology. 

12.  Determinations    of  Geographical  33.  Meteorological  Observations. 

Positions.  34.  History  of  Astronomy. 

13.  Metrology.  35.  Astronomical  Biography. 

14.  Earthquake  Literature,  Geography,  36.  Astronomical  Bibliography. 

and  Geology.  37.  Comets,  Meteors. 

15.  Refraction.  38.  Spectroscopy. 

16.  The  Sun,  Zodiacal  Light.  39.  Photography. 

17.  Solar  Eclipses.  40.  Star  Maps. 

18.  The    Moon,     Occultations,  Lunar  41.  Geographical  Maps. 

Theory.  42.  Time  Services. 

19.  Transits  of  Inferior  Planets.  43.  Price  Lists  of  Instruments. 

20.  Planets  and  Satellites.  44.  Photographs. 

21.  Fixed  Stars  in  General.  45.  History  of  the  Lick  Observatory. 

22.  New  and  Variable  Stars.  .               46.  Catalogues  of  Colleges. 

23.  Double  Stars.  47.  Miscellaneous. 

24.  Nebulae,  Clusters.  48.  Publisher's  Book  Lists. 

Also,  unnumbered  drawers: 

Topography  of  Mount  Hamilton  and  vicinity. 
Statistics  of  California. 
Statistics  of  the  United  States. 
Price  Lists  of   Supplies. 
University  of  California. 

If  the  books  or  pamphlets  on  a  given  subject  are  wanted,  they 
can  be  found  in  their  assigned  places;  if  the  works  of  a  given 
author  are  required,  their  titles  can  be  found  in  the  catalogue. 


6*  Catalogue  of  the 


The  hearty  thanks  of  the  Observatory  are  returned  to  the 
many  observatories,  learned  societies,  and  individuals  who 
have  presented  their  publications  to  the  library.  So  far  as  the 
editions  of  our  own  publications  are  sufficient,  they  have  been 
sent  in  exchange  for  such  gifts.  The  entries  in  the  catalogue 
will  serve  to  show  our  great  indebtedness  to  the  correspondents 
of  the  Observatory.  This  is  the  place,  also,  to  express  our  obli- 
gations to  the  Smithsonian  Institution,  which  transmits  our 
foreign  exchanges  free  of  cost. 

In  conclusion,  I  wish  to  point  out  that  the  isolated  position 
of  the  Lick  Observatory  renders  it  essential  that  a  large  library 
of  reference  should  be  available  to  the  astronomers,  whose 
work  is,  and  will  always  be,  related  to  many  different  depart- 
ments— as  Astronomy,  Mathematics,  Physics,  Chemistry,  Ge- 
odesy. The  equipment  of  the  institution  requires  to  be 
strengthened  in  this  direction  perhaps  more  than  in  any  other. 

EDWARD  S.  HOLDEN. 
MT.  HAMILTON,  July  1,  1890. 


Lick  Observatory  Library.  7* 


CATALOGUE  OF  THE  LIBRARY. 


A.  (F.  H.) :  The  Libraries  of  California,  by  F.  H.  A.  San  Fran- 
cisco, 1878.  8vo. 

ABBE  (C.) :  Report  *  *  *  (on)  the  Meteor  of  December  24, 
1873.  Washington,  1877.  8vo.  P. 

ABBOT  (H.  L.):  Practical  Astronomy  at  the  Engineer  School 
of  Application,  at  Willet's  Point,  N.  Y.,  1882  [Programme 
of  instruction].  Willet's  Point,  1882.  8vo.  P. 

:  [Geographical  Position  of  Willet's  Point,  N.  Y.]  6  num- 
bers. 8vo.  P. 

and  RAYMOND  (C.  W.):  Observations  at  the  recent  tran- 
sit of  Venus  (1882).  Willet's  Point,  n.  d.  4to.  P. 

ABERCROMBY  (R.):  Weather.     New  York,  1887.     8vo. 

ABNEY  (W.  de  W.):  A  Treatise  on  Photography.  London, 
1888.  16mo. 

ABO  (observatory):  Observationes  Astronomic^  in  specula 
Universitatis  Litterarise  Fennicse  factse.  3  vols.  1830-32. 
Vol.  1,  1824-25;  vol.  2,  1826-27;  vol.  3,  1828.  Helsing- 
fors,  1830.  folio. 

ACTA  MATHEMATICA:  Part  1.     Stockholm,  1882.     4to.     P. 

ADAMS  (F.  A.):  Arithmetic.     Lowell,  1847.     12mo. 

ADAMS  (J.  C.):  An  explanation  of  the  irregularities  in  the 
motions  of  Uranus.  London,  1846.  8vo. 

ADELAIDE  (observatory):  Meteorological  observations.  [Trans- 
ferred to  the  University  Library,  Berkeley.] 

AGAMENNONE  (G.):  II  terremoto  nel  vallo  Cosentino  (1887). 
Rome,  1888.  folio.  P. 

:  Sopra  la  correlazione  dei  Terremoti  con  le  perturbazioni 

magnetiche.     Rome,  1890.     8vo.     P. 

AIRY  (G.  B.):  Mathematical  Tracts.     Cambridge,  1831.     8vo. 

:  Gravitation.     London,  1834.     8vo. 

9 


8*  Catalogue  of  the 


AIRY  (Gr.  B.):  On  the  determination  of  the  Orbits  of  Comets 
from  observations.     London,  1839.     4to.     P. 
Catalogue  of  1439  stars  for  1840. 
Catalogue  of  2156  stars  (12  year). 
Catalogue  of  1576  stars  (6  year). 
Catalogue  of  2022  stars  (7  year). 
Catalogue  of  2760  stars  (7  year). 

Catalogue  of  2263  stars  (9  year).    6  vols.   London,  1843- 
76.     4to. 

Longitude  of  Valentia.     London,  1846.     4to. 
An  elementary  treatise  on  Partial  Differential  Equations. 
London,  1873.     12mo. 

Report  on  the  Observations  of  the  Transit  of  Venus,  1874. 
Parliamentary  paper.)     London,  1877.     folio.     P. 
Numerical  Lunar  Theory.     London,  1 886.     4to. 
Instructions  to  Observers  (of  the  Transit  of  Venus,  1874). 
London,  n.  d.     4to.     P. 

The  Transit  of    Venus,  1874  and  1882.     London,  n.  d. 
8vo.     P. 

Reports   of   the    Astronomer-Royal,    1836-64,    1865-79. 
2  vols.     London.     4to. 

ALBANY   (Dudley  Observatory):    Annals.     Vol.   I    (1866J,   II 
(1871).     Albany.     8vo. 

:  Report  for  1863,  1877.     Albany.     8vo.     P< 

ALBINI  (G.) :  The  Sun's  true  bearing,  or  Azimuth  tables.    Milan, 

1876.     4to. 
ALBRECHT    (Th.):    Formeln   und    Huelfstafeln.      2d    edition. 

Leipzig,  1879.     8vo. 

ALDIS  (W.  S.):  A  Text-Book  of  Algebra.    Oxford,  1877.    12mo. 
ALEXANDER  (S.):    *     *     *     Certain   harmonies   of  the  Solar 
System.     Washington,  1875.     4to.     P. 

[ ]:   (Biography  of.)     n.  p.,  n.  d.     8vo.     P. 

ALVORD  (B) :  The  tangencies  of  circles  and  spheres.     Washing- 
ton, 1855.     8vo. 

(The)    AMERICAN   ALMANAC:    For   1830,   1858,   1881.     3   vols. 
Boston  and  Washington.     16mo. 

:  And  Treasury  of  Facts,   etc.     4   vols.,   1878-79-80-81. 

New  York  and  Washington,  1878-81.     16mo. 


Lick  Observatory  Library.  9* 

AMERICAN  ASSOCIATION  FOB  THE  ADVANCEMENT  OF  SCIENCE:  See 
Salem. 

AMERICAN  EPHEMERIS  AND  NAUTICAL  ALMANAC:  For  the  years 
1855-6-7-8-9,  1860-1-2-3-4-5-6-7-8-9,  1870-1-2-3-4-5- 
6-7-8-9,  1880-1-2-3-4-5-6-7-8-9,  1890-1-2-3.  Washing- 
ton. 8vo. 

AMERICAN  JOURNAL  OF  SCIENCE:  Series  I;  Vol.1  (1818-9),  (13- 
14-15),  (28-29),  (30-35-36-39),  (31-32),  (33-34),  (37-38), 
(40-41),  (42-43),  (44-45),  (46-47),  (48-49).  Series  II; 
Nos.  (1-2-3-4)  (1846),  (8-11-12-15-18),  (21-22-23-24- 
f  25-26-27).  Series  III;  Vol.  10  (1875),  (25-26)  (1883), 
(27-28)  (1884),  (29-30)  (1885).  New  Haven,  1818-1885. 
8vo. 

AMERICAN  METEOROLOGICAL  JOURNAL:  V  (1888),  VI.  Ann 
Arbor.  8vo. 

AMSTERDAM  (Royal  Society  of  Sciences) :  Verslagen  en  Mededeel- 
ingen.  Series  II,  Vols.  16-17-18-19-20;  Series  III,  Vols. 
1-2-3-4.  Amsterdam,  1881-  8vo. 

ANDING  (E.):  Photometrische  Untersuchungen  ueber  die  Ver- 
finsterungen  der  Jupiters  trabanten.  Munich,  1889.  4to.  P. 

ANDRE  (C.):  Rapport  sur  le  passage  de  Mercure  sur  le  soleil, 
(1878).  Paris,  1881.  8vo.  P. 

:  Sur  le  ligament  lumineux  des  passages,  etc.,  des  Satel- 
lites de  Jupiter.  Paris,  n.  d.  4to.  P. 

:  Passage  de  Venus,  1874.     Paris,  n.  d.     4to. 

et  RAYET  :  LJ  Astronomic  pratique  et  les  observatoires  en 

Europe  et  en  Amerique.  Vols.  I,  II,  III,  IV,  V.  Paris, 
1874-78.  12mo. 

ANGOT  (A.):  Sur  F  application  de  la  photographic  a  1'observa- 
tion  du  passage  de  Venus.  I  (1877),  II  (1877).  2  num- 
bers. Paris,  1877.  4to.  P. 

ANGUIANO  (A.):  Primera  Memoria  del  Observatorio  Nacional. 
Mexico,  1880.  8vo.  . 

:  Viaje  a  Europa  en  Comision  Astronomica.  Mexico,  1882. 

8vo.  P. 

:  Longitud  del  Observatorio  Nacional  Mexicano.  Mexico, 

1886.  8vo.  P. 

:  Coordenadas  geograficas  (in  Mexico).  Mexico,  1886. 

8vo.  P. 


10*  Catalogue  of  the 


ANN  ARBOR  (observatory):  Report  for  1880.     Ann  Arbor,  1881. 

8vo.     P. 
ANNALES  DE  CHIMIE  ET  DE  PHYSIQUE:  Series  III,  vols.  52,  53, 

54  (1858),  bound  in  1  vol.     Paris,  1858.     8vo. 
ANNALS  OF  MATHEMATICS:  Vols.  I,  II,  III,  IV,  bound  in  1  vol. 

University  of  Va.,  1884-88.     4to. 

:  Vol.  V  (current). 

(The)  ANNUAL  STATISTICIAN:  1889.     San  Francisco,  1889.     8vo. 
ANONYMOUS:    Disputes  in  the  Royal  and  Royal  Astronomical 

Societies.     London,  1855.     8vo.     P. 
ANTHON  (C.)^  See  Dictionary. 
ANTHONY  (E.  and  H.  T.):  The  International  Bulletin  of    *     * 

[Photography].     I  (1888),  III  (1890).     New  York.     8vo. 
ANTON  (F.):   Specielle  Stoerungen  und  Ephemeriden   fur  die 

Planeten  (114)  und  (154).     Vienna,  1887.     8vo.     P. 
:  Bestimmung  der  polhoehe  des    *    *    *    observatoriums 

in  Triest,  etc.     Vienna,  1889.     8vo.     P. 
APELT  (E.  F.):  Die  Reformation  der  Sternkunde.     Jena,  1852. 

8vo. 

APPLETON  (D.):  See  Encylopsedia. 
ARAGO  (F.):  Astronomic  Populaire.     Vols.  1,  2,  3,  4.     Paris, 

1854-57.     8vo. 

:  Oeuvres.     2d  edition;  17  vols.     Paris,  1865.     8vo. 

ARGELANDER  (F.  W.  A.):    DLX  stellarum  fixarum  positiones 

mediae  ineunte  anno,  1830.     Helsingfors,  1835.     4to. 
:  Uranometria   Nova.     1  vol.  text,  1  vol.  atlas.     Berlin, 

1843. 
:   Anhang  to  Bonn  Observations,    Vol.  II.      (Reduction 

Tables  for  Southern  Zones.)     Bonn,  1852.     32mo. 
:  De  Stella  Beta  Lyrae  Variabili  Commentatio  altera.  Bonn, 

1859.     4to.     P. 

:  See  Abo;  see  Bonn. 

ARMAGH  (observatory):    Second    Armagh  Catalogue    of  3300 

Stars  for  1875,  prepared  by  J.  L.  E.  DREYER.    Dublin,  1886. 

8vo. 

:  See  DREYER. 

[ASHBURNER  (W.)]:  Memorial.   San  Francisco,  1887.    8vo.   P. 


Lick  Observatory  Library.  11* 

ASTEN  (E.  von):  Ueber  die  Erscheinung  des  ENCKE'  schen 
Cometen  in  J.  1875,  etc.  St.  Petersburg,  1874.  8vo.  P. 

ASTRAND  (J.  J.):  Katalog  [over]  Bergens  Observatoriums 
Bibliothek.  Bergen,  1879.  8vo.  P. 

:  Om  en  Auxiliaertabel  til  Losning  af  KEPLER'S  Problem. 

Bergen,  1887.  4to.  P. 

ASTRONOMICAL  JOURNAL:  Vols.  VII,  VIII,  IX  (current).  Boston, 
1886.  4to. 

(The)  ASTRONOMICAL  REGISTER:  Vol.  24  (Nos.  277-288),  1886. 
No.  287  missing.  London,  1886.  8vo. 

:  General  Index  to  the  first  20  vols.,  by  F.  W.  LEVANDER. 

London,  1883.  8vo. 

L'ASTRONOMTE:  Vol.  I  (Nos.  8,  10),  II  (9,  10, 11,  12),  III  (com- 
plete), IV  (1,  2,  3,  4,  5,  6,  7,  8,  9,  10-12),  V  (1,  2,  3,  -  5,  6,- 
10,-12),  VI  (-2,-4-8,  9, 10,  11),  VII  (1,  2,  3,  -,  5,  6,  7-9, 10, 
11,  12).  Paris.  8vo. 

ASTRONOMISCHE  MlTTHEILUNGEN:    Von  Dr.  RUDOLF  WOLF.       Vol. 

V  (Nos.  41-50),  1876-79;  VI  (51-60),  1880-88;  VII  (61- 
70),  1884-87;  also,  Nos.  71,  72,  73,  74.  Zurich.  8vo. 

ASTRONOMISCHE  NACHRICHTEN:  Vols.  (1,2),  (3,4),  (5,6),  (7,8), 
(9,  10),  (11,  12),  (13,  14),  (15,  16),  (17,  18),  (19,  20),  (21, 
22),  (23,  24),  (25,  26),  (27,  28),  (29,  30),  (31,  32),  (33,  34), 
(35,  36),  (37,  38),  (39,  40),  (41,42),  (43,  44),  (45,46), 
(47,  48),  (49,  50),  (51,  52),  (53,  54),  (55,  56),  (57,58), 
(59,  60),  (61,  62),  (63,  64),  (65,  66),  (67,  68),  (69,  70), 
(71,  72),  (73,  74),  (75,  76),  (77,  78),  (79,  80),  (81,  82), 
(83,  84);  also,  Vols.  79,  80-1-2-3-4-5-6-7-8-9,  90-1-2-3- 
4_5_6-7-8-9, 100-1-2-3-4-5-6-7-8-9, 110-1-2-3-4-5-6-7- 
8-9,  120-1-2-.  Altona  and  Kiel,  1823-90.  4to.  Also, 
Registers  A.  N.  1-80,  bound  in  3  vols.  4to. 

ASTRONOMISCH-NAUTISCHE  EPHEMERIDEN:  Fur  das  Jahr,  1890- 
91.  Trieste,  1889.  8vo. 

ASTRONOMICAL  NOTICES:  By  F.  BRUENNOW.  Nos.  1-20  (1  vol.). 
Ann  Arbor,  1858.  8vo. 

ANTHONY'S  PHOTOGRAPHIC  BULLETIN:  From  March  22,  1890,  to 
.  New  York.  8vo.  P. 

ATKINSON  (E.):  Elementary  Treatise  on  Physics  [translated, 
etc.,  from  GANOT].  New  York,  1886.  8vo. 


12*  Catalogue  of  the 


AUWERS  (A.):  Untersuchungen  ueber  Veraenderliche  Eigenbe- 
wegungen.  Erster  Theil.  Koenigsberg,  1862.  4to.  P. 

:  Parallaxen-Bestimmungen  mit  dem  Koenigsberger  Helio- 

meter.  Kiel,  1863.  4to.  P. 

:  Neue  Reduction  der  BRADLEY'  schen  Beobachtungen, 

1750-62;  Vols.  II,  III.  St.  Petersburg.  4to. 

:  See  Berlin  (Transit  of  Venus  Commission). 

BACHE  (A.  D.):  Report  on  Education  in  Europe.  Philadelphia, 
1839.  8vo. 

:  Notes  on  the  use  of  the  Zenith  Telescope,  etc.  New 

Haven,  1852.  8vo.  P. 

:  Magnetic  and  Meteorological  Observations  at  Girard  Col- 
lege; Parts  I,  II,  III,  IV,  V,  VI,  VII,  VIII,  IX,  X,  XI,  XII. 
Washington,  Smithsonian  Institution,  1859.  4to. 

:  Magnetic  Survey  of  Pennsylvania  in  1840-41.  Wash- 
ington, Smithsonian  Institution,  1863.  4to. 

BACKLUND  (0.):  Zur  Theorie  des  ENCKE' schen  Cometen.  St. 
Petersburg,  1881.  folio.  P. 

:  Untersuchungen  ueber  die  Bewegung  des  ENCKE'  schen 

Cometen,  1871-81.  St.  Petersburg,  1884.  folio.  P. 

:  Zur  Entwickelung  der  Stoerungsfunction.  St.  Peters- 
burg, 1884.  folio.  P. 

:  Comet  ENCKE,  1865-85.   St.  Petersburg,  1886.     folio.     P. 

:  Dr.  HARZER'S  Untersuchungen  ueber  einen  speciellen  Fall 

des  Problems  der  drei  Koerper,  etc.  St.  Petersburg,  1886. 
8vo.  P. 

:  Studien  ueber  den  Sterncatalog  "  Positions  moyennes  de 

3542  etoiles,  etc."  (Also)  Zusatz.  St.  Petersburg,  1887. 
8vo.  P. 

:  Bermerkung  ueber  das  Auftreten  von  hyperelement- 

aeren  Gliedern  in  der  Stoerungstheorie.  No.  1.  St. 
Petersburg,  1888.  8vo.  P. 

:  Ueber  die  herleitung  der  im  8  Bande  des  "Observations 

de  Poulkova  "  enthaltenen  Sterncataloge,  etc.  St.  Peters- 
burg, 1888.  folio.  P. 

:  Ueber  einige  von  WINNECKE,  am  Pulkowaer  Meridian 

Kreise  (1861-3)  augestellte  Beobachtungen.  St.  Peters- 
burg, 1890.  8vo.  P. 

:  Ueber  die  Kleinen  Divisoren  bei  den  elementaren  Glie- 
dern in  der  Theorie  der  Planeten  bewegungen.  Kiel,  1889. 
4to.  P. 


Lick  Observatory  Library.  13* 

BAEYER  (J.  J.):  Ueber  die  Strahlenbrechung.  St.  Petersburg, 
1860.  folio.  P. 

:  Ueber  die  Aufloesung  grosser  Sphaeroidischer  Dreiecke. 

Altona,  1864.  4to.  P. 

:  Uebersicht  der  bis  jetzt  in  Thiiringen  ermittelten  Loth- 

ablenkungen.  Berlin,  1874.  8vo.  P. 

BAGAY  (V.):  Nouvelles  Tables  Astronomiques  (bound  in  two 
volumes).  Paris,  1829.  4to. 

BAILY  (F.):  Life  of  FLAMSTEED,  to  which  is  added  his  British 
Catalogue  of  Stars.  London,  1835.  4to. 

:  The  Catalogue  of  [8377]  Stars  of  the  British  Association 

for  the  Advancement  of  Science.  London,  1845.  4to. 

:  A  Catalogue  of  9766  Stars  from  the  Observations  of  the 

Abbe  de  LACAILLE.  London,  1847.  8vo. 

:  A  Catalogue  of  [47390]  Stars  in  the  Histoire  Celeste 

fran$aise  of  LALANDE.  London,  1847.  8vo. 

BAKHUYSEN  (H.  G.  v.  d.  S.):  Untersuchungen  ueber  die  Rota- 
tionszeit  des  Planeten  Mars.  Leiden,  n.  d.  4to.  P. 

:  Beschreibung  eines  Apparats  zur  bestimmung  des  abso- 

luten  personlichen  Fehlers,  etc.  The  Hague,  n.  d.  4to. 

:  See  SCHROETER. 

and  BASSOT:  Determination  de  la  difference  de  Longitude 

entre  Leyde  et  Paris.  Paris,  1 889.  4to.  P. 

BALL  (L.  de):  Recherches  sur  1'orbite  de  la  planete  (181). 
Brussels,  1887.  4to.  P. 

:  Die  Untersuchungen  MONTIGNY'S  ueber  das  Funkeln  der 

Sterne.  Berlin.  8vo.  P. 

BALL  (R.  S.):  Extension  of  the  Theory  of  Screws  to  the  Dy- 
namics of  any  Material  System.  Dublin,  1881.  4to.  P. 

:  Elements  of  Astronomy.     London,  1886.     12mo. 

" :  The  Story  of  the  Heavens.     London,  1887.     8vo. 

:  Krakatoa  (from  Contemporary  Review,  Nov.,  1889).  Lon- 
don, 1889.  8vo.  P. 

BALTIMORE  (Johns  Hopkins  University):  Circulars — I  (Nos. 
1-17)  (1879-82);  II,  III,  IV  (Nos.  18-67)  (1882-85);  V, 
VI,  VII,  VIII  (Nos.  43-75)  (1885-89).  3  vols.  Balti- 
more. 4to. 

BARCLAY  (J.  G.):  Astronomical  Observations  during  the  Years 
1865-69  (Vol.  II).  London,  1870.  4to. 


14*  Catalogue  of  the 


BARKER  (G.  F.):  See  DRAPER. 

BARLOW  (P.):     Tables   of   squares,  cubes,  square  roots,  cube 

roots,  reciprocals  of   all   integer   numbers   up   to   10000. 

London,  1882.     12mo. 
BARNARD    (E.   E.):    The  nebula  G.  C.  2091.     London,  1889. 

8vo.     P. 
:  Observations  of  the  Eclipse  of  Japetus,  1889,  November 

1.     London,  1890.     8vo.     P. 
BARNARD  (J.  G.):    Problems  of  Rotary  Motion  presented  by 

the  Gyroscope,  etc.     [Bound  with  other  Memoirs.]     Wash- 
ington, 1871.     4to. 
BARTON    (S.    M.):    BELLAVITIS'     method    of    equi-pollencies. 

Charlottesville  (1885).     8vo.     P. 
BARTHOLTNI    (E.):     ERASMI    BARTHOLINI     De    Cometis   Anni 

MDCLXIV  &  MDCLXV  Opusculum.     Hafnise,  1665.    4to. 
BARUS  (C.):   Subsidence  of  Fine  Solid  Particles  in  Liquids. 

Washington,  1886.     8vo.     P. 
and    STROUHAL     (V.):     The    Electrical    and    Magnetic 

Properties   of   the    Iron    Carburets.     Washington,    1885. 

8vo.     P. 
:  Physical  Properties  of  the  Iron  Carburets.     Washington, 

1886.     8vo.     P 

BATAVIA  (observatory):  Meteorological  observations.     [Trans- 
ferred to  the  University  Library,  Berkeley.] 
BATTERMANN  (H):  Beitraege  zur  astronomischen  Aberrations- 

lehre.     Berlin,  1881.     8vo.     P. 
:  Untersuchungen  ueber  die  Gestalt  der  Bilder,  etc.,  aus- 

serhalb  der  optischen  Axe  von    astronomischen    Instru- 

menten.     Kiel,  1889.     4to.     P. 
BAUERNFEIND   (C.    M.):    Elemente   der   Vermessungs   Kunde. 

Vols.  I,  II.     Stuttgart,  1879.     8vo. 
BAUSCHINGER  ( J.) :  Ueber  die  Biegung  von  Meridian-fernrohren. 

Munich.  1888.     4to.     P. 

BAYER  (J.):  Uranometria.     Ulm,  1661.     folio. 
BEAUJEAN  (A.):  See  Dictionary. 
BECKER  (E.):  Resultate  aus  Beobachtungen  von  521  BRADLEY' 

schen  Sternen  am  grossen  Berliner  Meridian  Kreise.     Ber- 
lin, 1881.     4to.     P. 


Lick  Observatory  Library.  15* 

BECKER  (G.  F.) :  Geometrical  form  of  Volcanic  Cones,  etc.    New 

Haven,  1885.     8vo.     P. 
:  Notes  on  the  stratigraphy  of  California.     Washington, 

1885.     8vo.     P. 
:  An  elementary  proof  of  the  Earth's  rigidity.  New  Haven, 

1890.     8vo.     P. 

BECKETT  (E.):  Clocks,  Watches,  and  Bells.  London,  1883.    8vo. 
BECQUEREL  (A.  C.):  Traite  de  Physique.     2  vols.     Paris,  1842- 

44.     8vo. 
and  BECQUEREL   (E.):    Traite  d'Electricite.     Vol.    1   and 

Vol.  3.     Paris,  1855-56.     8vo. 
BEEBE    (W.)    and   PHILLIPS    (A.  W.):    The   Orbit  of  SWIFT'S 

Comet,   1880   V,   determined   by   GIBBS'  Vector   method. 

Cambridge,  1889.     4to.     P. 
BEER    (W.)   and  MAEDLER    (J.    H.):     Mappa  Selenographica 

Editio  genuina.     Berlin,  1834.     folio. 

:  Der  Mond.     Berlin,  1837.     4to. 

:  Beitraege  zur  physichen  Kenntniss  der  himmlischen 

Koerper  im  Sonnensystem.     Weimar,  1841.     4to. 
BEHRMANN    (C.):  Atlas   des   Sudlichen   Gestirnten   Himmels. 

1  vol.  text,  1  vol.  atlas.     Leipzig,  1874. 
BEIMA  (E.  M.):  De  Annulo  Saturni.     Leyden,  1842.     4to. 
BENTLEY   (J.):  A  Historical  View  of  the  Hindu  Astronomy. 

Calcutta,  1823.     4to. 
BERGHAUS    (H.):  Physikalischer   Atlas.      Parts  1-7.      Gotha, 

1849-52.     folio. 

:  Chart  of  the  World  on  Mercator's  projection,     llth  edi- 
tion.    Gotha,  1886.     Wall  map. 
BERKELEY  (University  of  California):  Annual  Reports,  1875-80 

and  1884-87,  bound  in  1  vol.    Sacramento.    8vo. 
:  Biennial  Reports,  1872-9,  bound  in  1  vol.     Sacramento. 

8vo. 
:  Registers  for  the  years  1871,  1875-82,1884-6,  bound  in 

1  vol.     Sacramento.     8vo. 
:  Annual  Report  of  the  Secretary  for  the  year  ending  June 

30,  1881-82-83.     3  vols.     Sacramento.     8vo. 
:  Registers  for  1882-3,  1886-7.     2  vols.     Report,  1879-80, 

1881-2,  1882-4,  1886, 1887.     5  vols.     Sacramento.     8vo. 


16*  Catalogue  of  the 


BERKELEY  (University  of  California):  Library  Bulletins,  1,  3-9, 
bound  in  1  vol.  Sacramento.  8vo. 

:  Bulletins,  Nos.  1-36,  bound  in  1  vol.     Sacramento.     8vo. 

:  The  Blue  and  Gold.  Vols.  XII,  XIII.  San  Francisco. 

8vo. 

:  Formal  Recognition  of  the  Transfer  of  the  Lick  Observa- 
tory to  the  Board  of  Regents  of  the  University,  Berkeley, 
Wednesday,  June  27,  1888.  Sacramento,  1888.  8vo.  P. 

BERLIN  (Academy  of  Sciences):  Dissertations  sur  la  theorie 
des  Cometes,  etc.,  by  UONDORCET,  TEMPELHOFF,  and  HEU- 
NERT.  Utrecht,  1780.  4to. 

:  Abhandlungen  der  mathematischen  Klasse  aus  den 

Jahren,  1804-11.  Berlin,  1815.  4to. 

:  Akademische  Sternkarten.  1  vol.  text,  and  atlas.  Ber- 
lin, 1859.  folio. 

:  Abhandlungen,  1888.     4to. 

:  Sitzungsberichte,  1888.     8vo. 

BERLIN  (Association  Geodesique  Internationale):  Comptes-Ren- 
dus,  1878-79.  Berlin.  4to.  P. 

BERLIN  (Deutsche  Naturforscher  und  Aerzte) :  Katalog  zur  wis- 
senschaftlichen  Ausstellung  der  59  Versammlung.  Berlin, 
1886.  8vo.  P. 

BERLIN  (Gesellschaft  Urania) :  Ueber  die  Entwickelung  und  die 
Ziele  der  Gesellschaft  Urania.  Berlin,  1888.  8vo.  P. 

:  Himmel  und  Erde.  Vol.  I  (1889),  II  (current).  Berlin. 

8vo. 

BERLIN  ( Jahrbuch) :  Mittlere  Oerter  fur  1874.0  von  539  Sternen, 
etc.  Berlin,  1874.  8vo.  P. 

:  Jahrbuch  for  1882-3-4-5-6-7-8-9, 1890-1.  6  vols.  Ber- 
lin. 8vo. 

BERLIN  (observatory):  Beobachtungs-Ergebnisse.  See  BECKER, 
KusTNER3  MARCUSE. 

:  Astronomische  Beobachtungen.  Vols.  1-2  (1840-44),  3-4 

(1848-57),  5  (1884).  Berlin,  1840-84.  folio. 

BERLIN  (K.  Preussiche  Geodaetische  Institut):  Veroffentlich- 
ungen.  Astronomisch-Geodaetische  Arbeiten,  I  Ordnung. 
Berlin,  1889.  4to.  P. 

BERLIN  (Transit  of  Venus  Commission) :  Die  Venus-Durchgange 
1874  und  1882  (edited  by  A.  AUWERS).  Vols.  II,  III,  IV. 
Berlin,  1889,  etc.  4to. 


Lick  Observatory  Library.  17* 

BEBNOUILLI  (John):  -Opera  Omnia.     4  vols.     Lausanne,  1742. 

4to. 

BERTELLI  (T.):  Risposta,  etc.,  le  osservazioni  microsismiche  in 
occasione  del  terremoto  d'Ischia  del  1883.  Rome,  1885. 
8vo.  P. 

BERTRAND  (J.):  Calcul  des  Probabilites.     Paris,  1889.     8vo. 
BESANgoN   (observatory):    Premier   Bulletin   Chronometrique. 

Besanc,on,  1889.     4to.     P. 

BESSEL  (F.  W.) :  Fundamenta  Astronomise.  Koenigsberg,  1818. 
folio. 

Untersuchungen  liber  die  Lange  des  einfachen  Secunden- 
pendels.     Berlin,  1829.     4to. 

Tabulae  Regiomontanae.     Koenigsberg,  1830.     8vo. 
Astronomische  Untersuchungen.     2  vols.     Koenigsberg, 
1841-42.     4to. 

Populare  Vorlesungen.     Hamburg,  1848.     8vo. 
Abhandlungen     *     *     *     herausgegeben  von  R.  ENGEL- 
MANN.     Vols.  I,  II,  III.     Leipzig,  1875-6.     4to. 
Recensionen.     Leipzig,  1878.     8vo. 

andOLBERs:  Briefwechsel.    Vols.  1,2.   Leipzig,  1852.   8vo. 

and  GAUSS:  Briefwechsel.     Leipzig,  1880.     8vo. 

:  See  WEISSE. 

BIANCHI  (G.):  Osservazioni  Fondamentali  per  una  revista 
*  *  al  Catologo  delle  stelle  del  PIAZZI.  Modena,  1841.  4to. 

:  See  MODENA. 

BIBLE:  The  English  Version  of  the  Polyglott  Bible.  London, 
1823.  16mo. 

BlBLIOTHECA    HlSTORICO-NATURALIS,    ETC.:      (1875,     1880,     1881, 

1882  (ii),  1883),  1  vol.;  (1884,  1885,  1886,  1887),  1  vol. 
Gottingen.  8vo. 

BIGELOW  (F.  H.):  Solar  Vortices.     Salem,  1887.     8vo.     P. 

:  The  Solar  Corona  discussed  by  Spherical  Harmonics. 

Washington,  1889.  4to.  P. 

BIOT  (J.  B.):  Sur  les  Refractions  Astronomiques.  Paris,  1839. 
8vo. 

and  ARAGO  (F.):  Recueil  d'observations  Geodesiques  As- 
tronomiques et  Physiques.  Paris,  1821.  4to. 

BIRMINGHAM  (J.):  The  Red  Stars,  Observations  and  Catalogue. 
Dublin,  1877.  4to. 


18*  Catalogue  of  the 


BISHOP  (G-.):  Astronomical  Observations  taken  at  the  Observa- 
tory, South  Villa,  Regents  Park,  London,  during  the  years 

1839-51.     London.,  1852.     4to. 
BLACK  (A.  and  C.):  General  Atlas  of  the  World.     Edinburgh, 

1854.     folio. 
BLANCHINI  (F.):  Hesperi  et  Phosphori  Nova  Phenomena,  etc. 

Rome,  1728.     folio. 
:  Astronomica,  ac  Geographicae   Observationes   Selectae. 

Verona,  1836.     4to. 
BLASERNA  (P.) :  Sull'  impiego  del  servizio  Geodynamico  in  Italia. 

Rome,  1888.     8vo.     P. 
BLASS  (F.):  Inest  EUDOXI  Ars  Astronomica  qualis  in  charta 

Aegyptiaca  superest  denno  edita  a  FRIDERICO  BLASS.    Kiel, 

1887.     4to.     P. 
BLUNT   (E.):    Description  of  BLUNT'S  dividing  engine.      New 

York,  n.  d.     4to.     P. 
BOBOULIEFF   (D.):    Dissipation  of   electricity  in  gases.      New 

Haven,  1874.     8vo.     P. 
BODE  (J.  E.):  Astronomisches  Jahrbuch,  1785-6-7-8  and  1800. 

Berlin.     8vo. 
BOEDDICKER    (0.):    Physical   appearance  of  the   PlaneF  Mars 

(1881).     Dublin,  1882.     4to.     P. 
:  Physical   appearance    of    the    Planet    Jupiter,    1880-1. 

Dublin,  1882.     4to.     P. 
:  On  the  changes  of  the  radiation  of  heat  from  the  Moon 

during    the    total   eclipse   of    1884,   etc.      Dublin,   1885. 

4to.     P. 
:  Observations    of    the    Planet   Jupiter.      Dublin,    1889. 

4to.     P. 
BOEHM  ( J.  G.) :  Beobachtungen  von  Sonnenflecken  und  Bestim- 

mung  der  Rotations  Elemente  der  Sonne.     Vienna,  [1850]. 

folio. 
BOEHMER  (G.  H.):    Report  on  Astronomical  Observations  for 

1886.     Washington,  1889.     8vo.     P. 
BOERGEN  (C.):  See  COPELAND. 
BOGUSLAWSKI  (G.  von):  Die  Kometen  und  ihre  Bedeutung  als 

Weltkoerper.     Stettin,  1857.     8vo.     P. 
:  On  the  use  of  a  new  micrometer.     London,  n.  d.     4to.    P. 


Lick  Observatory  Library.  19* 

BOHLIN   (K.):    Ueber  die  Bahnelemente  des  Saturnsatelliten 

Tethys.     Stockholm,  1885.     8vo.     P. 
:  Om  en  grupp  af  differential  eqvationer,  etc.     Stockholm, 

1887.  8vo.     P. 

:  Om  betydelsen  af  lefvande  kraftens  princip,  etc.  Stock- 
holm, 1887.  8vo.  P. 

:  En  generalisation  af  LAPLACE'S  undersokning  af  libra- 

tionen  i  planetteorien.  Stockholm,  1888.  8vo.  P. 

:  Recherches  sur  les  perturbations  de  la  comete  de  WIN- 

NECKE  (1809-19).  Stockholm,  1888.  4to.  P. 

:  Ueber  eine  neue  annaherungsmethode,  etc.     Stockholm, 

1888.  8vo.     P. 

BOLOGNA  (Academy  of  Sciences) :  Memorie.     Series  IV,  Vol.  III. 

Bologna,  1881.     4to. 
BOMME  (B.):   Proeve  eener  Berekening  der  Storingen  in  der 

Loopbaan  der  Komet  van  1264-1556,  etc.     (Amsterdam), 

n.  d.     4to.     P. 
BOND  (G.  P.) :  On  the  outline  of  the  head  of  the  Comet  of  1858. 

Boston,  1861.     8vo.     P. 
:  On  the  new  form  [GAUSS']  of  achromatic  object  glass. 

Cambridge,  1863.     8vo.     P. 

:  Account  of  the  Comet  II,  1861.     New  Haven.     8vo.     P. 

BONN  (observatory):  Astronomische  Beobachtungen.    Vols.  1-2- 

3_4_5_6-7-8.    Bonn,  1846-86.    4to.    Also,  Atlas  to  the  S.  D. 
BORDEAUX    (observatory):   Annales.     I   (1885),  II  (1887),  III 

(1887).     Paris.     4to. 
BOSCOVICH   (R.  J.):    De   Solis   ac   Lvnae   Defectibvs,  libri   v. 

London,  1760.     4to. 
Boss  (L.):   Decimations  of  Fixed  Stars.     Washington  (1877). 

4to. 
:  Observations  of  the  Transit  of  Mercury,  1878.     Albany, 

1878.     8vo.     P. 

BOSSANGE  (H.):  Catalogue  des  livres,  etc.,  qui  ont  ete  publics 
en  Allemagne  en  1845.  Paris,  s.  d.  12mo. 

BOSSERT  (J.):  See  SCHULHOFF. 

BOSTON  (American  Metric  Bureau):  The  Metric  Bulletin,  July, 
1876.  Boston,  1876.  8vo. 


20*  Catalogue  of  the 


BOSTON  (American  Academy  of  Arts  and  Sciences):  Memoirs 
(new  series),  Vol.  8,  pt.  2.  Boston,  1863.  4to.  Proceed- 
ings, new  series,  Vol.  16;  whole  series,  Vol.  24  (1889).  Bos- 
ton. 8vo. 

BOSTON  (Appalachian  Club):  Appalachia,  Vols.  I,  II,  III,  IV, 
V,  VI  (current).  8vo.  Also,  Registers  of  the  A.  Club.  16mo. 

BOUGUER  (P.):  La  Figure  de  la  Terre.     Paris,  1749.     4to. 

:  Traite  d'Optique  (edited  by  LACAILLE).     Paris,  1760.   4to. 

:  Justification  *  *  *  du  livre  de  la  figure  de  la  Terre. 

2d  edition.  Paris,  1809.  4to. 

[BOUSSINGAULT  (J.  B.  J.  D.)]:  See  LAUSSEDAT. 

BOWDITCH  (N.):  See  LAPLACE. 

BRADLEY  (J.):  See  AUWERS;  see  BESSEL. 

BRASSART  (E.):  II  Sismetrografo  a  tre  component!,  etc.  Rome, 
1888.  folio.  P. 

:  I  sismometri  presentemente  in  uso  nel  Giappone.  Rome, 

1888.  folio.  P. 

:  Sismoscopi.     Rome,  1888.     folio.     P. 

BREDICHIN  (Th.):  Sur  quelques  anomalies  apparentes  dans  la 
structure  des  Queues  cometaires.  Moscow,  1883.  8vo.  P. 

:  Histoire  de  1'hypothese  des  on  des  cosmiques,  etc:;  also, 

Supplement  a  1'histoire,  etc.  Moscow,  1883.  8vo.  P. 

:  Quelques  remarques  concernanfr  mes  recherches  sur  les 

cometes.  Moscow,  1884.  8vo.  P. 

:  Sur  les  anomalies  apparentes  dans  la  structure  de  la 

grande  Comete  de  1744.  Moscow,  1884.  8vo.  P. 

:  Sur  1'origine  des  Etoiles  filantes.    Moscow,  1888.    8vo.    P. 

:  Sur  Torigine  des  Cometes  periodiques.  Moscow,  1889. 

8vo.  P. 

BREITHAU.PT  (F.  W.):  Magazin  der  neuesten  mathematischen 
Instrumente,  etc.  Heft  VI.  Cassel,  1876.  4to.  P. 

BREMIKER  (C.):  Logarithmisch-trigonometrische  Tafeln  mit  5 
Decimalstellen.  Berlin,  1883.  8vo. 

:  See  CRELLE. 

BRENNAN  (M.  S.):  Astronomy,  new  and  old.  New  York,  1889. 
12mo. 

BRESLAU  (observatory):  Mittheilungen.     Breslau,  1879.     4to. 

BRESSE  ( — ):  Cours  de  Mecanique  Appliquee.  I,  II,  III, 
bound  in  1  vol.  Paris,  1865-6.  8vo.  Also,  Atlas. 


Lick  Observatory  Library.  21* 

BRESTER  (A.):  Essai  d'une  explication  Chimique  des  princi- 
paux  phe'nomenes  lumineux  stellaires.  Delft,  1888. 
8vo.  P. 

BRILL  (L.):  Catalog  mathematischer  modelle,  etc.  Darmstadt, 
1888.  8vo.  P. 

BRISBANE  (T.  M.) :  Catalogue  of  7385  Stars.    London,  1835.    4to. 

BRISBANE  (Chief  Weather  Bureau):  The  Queensland  Meteoro- 
logical Record,  published  by  C.  L.  WRAGGE.  [Transferred 
to  the  Library  of  the  University,  Berkeley.] 

BRISBANE  (Royal  Geographical  Society  of  Australia):  Publica- 
tions. Vol.  Ill,  part  2;  IV;  V,  parti.  Brisbane,  1889.  Svo. 

BRITISH  ASSOCIATION  FOR  THE  ADVANCEMENT  OF  SCIENCE:  See 
London. 

BROOKLYN  (American  Astronomical  Society):  Papers,  I,  II,  III 
(1885-88)  (all  published),  bound  in  1  vol.  n.  p.  Svo. 

BRUENNOW  (F.):  Sur  la  comete  elliptique  de  DE  Vico.  Amster- 
dam, 1848.  4to. 

:  Astronomical  Notices,  Nos.  1-20  (1  vol.).  Ann  Arbor, 

1858.  Svo. 

:  Tables  of  Victoria.     New  York,  1859.     4to.     P. 

:  Lehrbuch  der  Sphaerischen  Astronomie.  Berlin,  1871. 

Svo. 

BRUHNS  (C.):  Die  Astronomische  Strahlenbrechung.  Leipzig, 
€861.  Svo. 

:  J.  F.  ENCKE  Sein  Leben  und  Wirken.    Leipzig,  1869.    Svo. 

:  A  new  manual  of  logarithms  [7  figures].  Leipzig,  1881. 

Svo. 

and  FOERSTER  (W.):  Bestimmung  der  Laengen-DifFerenz 

zwischen  Berlin  und  Leipzig.  Leipzig,  1865.  4to. 

BRUNS  (H.):  Ueber  die  Rotation  eines  starren  Koerpers. 
Leipzig,  1885.  Svo.  P. 

:  Ueber  eine  aufgabe  der  Ausgleichungsrechnung.  -Leip- 
zig, 1886.  Svo.  P. 

:  Ueber  die  Integrale  des  Vielkorper-problems.  Leipzig, 

1887.  Svo.  P. 

:  Ueber  eine  Minimum saufgabe.     Leipzig,  n.  d.     Svo.     P. 

BRUSSELS  (Royal  Observatory):  Annuaire,  1881.     32mo.     P. 

BRYANT  (R.):  The  orbit  of  the  planet  Sappho.  London,  1889. 
Svo.  P. 


22*  Catalogue  of  the 


BUGGE  (T.):  Observations  astronomicse  annis  1781,  1782,  and 

1783    institute   in    Observatorio    Regio    Havniensi,   etc. 

Hauniae,  1784.     4to. 
BULLETIN  ASTRONOMIQUE:'  Vol.  Ill  (1886),  IV  (1887),  V  (1888), 

VI  (1889),  VII  (current).     Paris.     8vo. 
BURCKHALTER    (C.):    Total   Solar   Eclipse,   January   1,   1889. 

Northfield,  1889.     8vo.     P. 
BURDER    (G.    F.):    The   illumination   of  the   eclipsed    Moon. 

Bristol,  1888.     8vo.     P. 

BURNHAM  (S.  W.):  [First]  Catalogue  of  81  Double  Stars,  dis- 
covered with  a  6-inch  ALVAN  CLARK  Refractor.  London, 

1873.  8vo.     P. 

:  A  Second  Catalogue  of  New  Double  Stars,  discovered 

with  a  6-inch  CLARK  Refractor.    London,  1873.    Svo.    P. 
:  A  Third  Catalogue  of  76  New  Double  Stars,  discovered 

with  a  6-inch  ALVAN  CLARK  Refractor.      London,  1873. 

Svo.     P. 
:  A  Fourth  Catalogue  of  47  New  Double  Stars,  discovered 

with  a  6-inch  CLARK  Refractor.     London,  1874.     Svo.     P. 
:  A  Fifth  Catalogue  of  71   New  Double  Stars.     London, 

1874.  Svo.     P. 

:  Notes  in  reply  to  Sir  JOHN  HERSCHEL'S  "  Queries  Relative 

to  Double  Stars."  London,  1874.  -  Svo.  P. 

:  On  the  Duplicity  of  the  Principal  Star  of  Nu  Scgrpii. 

London,  1874.  Svo.  P. 

:  Seventh  Catalogue  of  New  Double  Stars.  New  Haven, 

1876.  Svo.  P. 

:  Double  Star  Discoveries  with  the  18^-inch  Chicago  Re- 
fractor. New  Haven,  1877.  8vo.  P. 

:  Ninth  Catalogue  of  New  Double  Stars,  discovered  with 

the  6-inch  refractor.  London,  1874.  Svo.  P. 

:  Beta  Leonis  and  B.  A.  C.  3992.     London,  1878.     Svo.     P. 

:  Double  Stars  discovered  by  Mr.  ALVAN  G.  CLARK.  New 

Haven,  1879.  Svo.  P. 

— — :  New  Double  Stars.     London,  1879.     Svo.     P. 

:  An  examination  of  the  double  star  measures  of  the  Bed- 
ford Catalogue.  London,  1880.  Svo.  P. 

:  Quadruple  Stars.     London,  1881.     Svo.     P. 

:  The  trapezium  of  Orion.     London,  1889.     Svo.     P. 


Lick  Observatory  Library.  23* 

BURNHAM  (S.  W.):  A  new  method  of  bright  wire  illumination 
for  position  micrometers.     London,  n.  d.     8vo.     P. 
[All  the  above  bound  in  1  volume.     8vo.] 

:  1.  Double  Star  Observations  made  at  Chicago  in  1877-8. 

2.  Double   Star    Observations    made    in   1878   and    1880 
(bound  in  1  vol.).     London.     4to. 

:  Hints  to  Double  Star  Observers  (from  English  Mechanic). 

n.  p.,  1880.     folio.     P. 

:  Report  to  the  Trustees,  etc.,  of  observations  made  on  Mt. 

Hamilton  with  reference  to  the  location  of  the  Lick  Ob- 
servatory.    Chicago,  1880.     4to.     P. 

:  Double  Star  Observations  made  in  1879  and  1880  (at) 

Chicago  (from  Memoirs,  R.  A.  S.).     London,  1883.     4to.    P. 

:  Double  Star  Observations  made  (at)  the  Lick  Observa- 
tory (from  A.  N.,  Vol.  123).  Kiel,  1889.  4to.  P. 

:  Double  Star  discoveries  and  Measures  made  at  the  Lick 

Observatory,  Aug.  1,  1888,  to  Aug.  1,  1889  (from  Proc.  A. 
A.  A.  S.).     Salem,  1890.     8vo.     P. 

BURRITT  (E.):  Star- Atlas,     n.  p.,  n.  d.     folio. 

BURTON  (C.  E.):  On  a  new  form  of  Ghost  micrometer,  etc. 
Dublin,  1880.  8vo.  P. 

BUSCHBAUM  (C.):  Untersuchungen  liber  die  Bahn  des  Kometen 
1886,  IX.  Goettingen,  1889.  4to.  P. 

BUSZCZYNSKI  (B.):  Ueber  die  Bahnen  der  am  11  Dez.,  1852,  und 
am  3  Dez.,  1861,  beobachteten  Meteore.  Halle,  1886. 
8vo.  P. 

BUTLER  (T.  B):  The  Philosophy  of  the  Weather.  New  York, 
1856.  8vo. 

CALIFORNIA:  Civil  Code.     Sacramento,  1871.     8vo. 

:  Code  of  Civil  Procedure.     Sacramento,  1871.     8vo. 

:  Penal  Code.     Sacramento,  1871.     8vo. 

:  Political  Code.     See  NEWMARK. 

CAMBRIDGE  (England)  (University  Observatory):  Astronomical 
Observations.  Vols.  XXI  (1861-5),  XXII  (1866-9).  Cam- 
bridge. 4to. 

CAMBRIDGE  (U.  S.)  (Harvard  College  Observatory):  Annals. 
Vols.  1  (i,  ii);  2  (-,  ii);  4,  5,  6,  7,  9,  10,  11,  12,  13  (i,  ii); 

14, ,  17,  18,  19   (i,  -);  20,  21  (i,  -);  22.     Cambridge, 

1856.     4to. 
10 


24*  Catalogue  of  the 


CAMBRIDGE  (U.  S.)  (Harvard  College  Observatory):  Reports  of 

the  Director;  39th  (1884);  40th;  ;  42d;  43d;  44th. 

Cambridge.  8vo.  P. 

:  Astronomical  Engravings  [set  not  complete].  Bos- 
ton. 4to.  P. 

:  HENRY  DRAPER  Memorial.  Annual  Report.  I 

(1887);  II  (1888);  III  (1889).  Cambridge.  4to.  P. 

CAMPIDOGLIO  (Rome)  (observatory):  Osservazioni Meteor  ologiche. 
[Transferred  to  University  Library,  Berkeley.] 

CANFIELD  (C.  W.):  The  American  Annual' of  Photography. 
New  York,  1887.  8vo. 

CAPE  OF  GOOD  HOPE:  Cape  of  Good  Hope  Observations,  Vol.  I. 
Magnetical,  1841-46.  London,  1851.  4to. 

CAPE  OF  GOOD  HOPE  (Royal  Observatory):  Annals  (in  parts 
separately  indexed  under  authors). 

(observatory):  Observations  of  the  Great  Comet,  1882,  II. 

n.  p.,  n.  d.  4to.  P. 

:  Results  of  Meridian  Observations.  1879-80-81  (1 

vol.);  1882-83-84  and  part  of  1885  (1  vol.).  s.  1.,  s.  d.  8vo. 

:  See  GILL.     See  HERSCHEL.     See  STONE. 

CAPRON  (E.  S.):  History  of  California.     Boston,  1854,-  12mo. 

CAPRON  (J.  R.):  Aurorse;  their  characters  and  Spectra.  Lon- 
don, 1879.  4to. 

CARL  (P.):  Die  Principien  der  astronomischen  Instrumenten- 
Kunde.  Leipzig,  1863.  8vo. 

:  Repertorium  der  Com eten- Astronomic.  Munich,  1864. 

8vo. 

CARR  (G.  S.):  A  synopsis  of  elementary  results  in  Pure  Mathe- 
matics. London,  1886.  8vo. 

CARRINGTON  (R.  C.):  The  positions  of  twenty  polar  stars  as 
determined  at  Red  hill.  London,  1855.  8vo.  P. 

:  Catalogue  of  3735  Circumpolar  Stars.  London,  1857. 

folio. 

:  Information  and  suggestions  *  *  *  Eclipse  of  the 

Sun,  September  7,  1858.  London,  1858.  8vo.  P. 

:  On  Dr.  SOEMMERING'S  Observations  of  the  Solar  Spots, 

1826-29.  London,  1860.  8vo.  P. 

:  Observations  of  the  Spots  on  the  Sun  from  Nov.  9,  1853, 

to  March  24, 1861.  London,  1863.  4to. 


Lick  Observatory  Library.  25* 

CARSON  (Nevada)  (State  Weather  Service):  Reports.  [Trans- 
ferred to  University  Library,  Berkeley.] 

CASSINI  (J.  D.):  Abrege  des  observations  et  des  reflexions  sur 
la  Comete  de  1680  et  168J .  Paris,  1681.  4to. 

CASSINI  (Jaques):  Elements  d'Astronomie.     Paris,  1740.     4to. 

:  Tables  Astronomiques.     Paris,  1740.     4to. 

CASSINI  (J.  D.):  Voyage  fait  par  ordre  du  Hoi  en  1768,  Pour 
eprouver  les  Montres  Marines  inventees  par  M.  LE  ROY. 
Paris,  1770.  4to. 

CASSINI  DE  THURY  (G.  F.):  La  Meridienne  de  1'observatoire 
Royal  de  Paris,  etc.  Paris,  1744.  4to. 

CASWELL  ( A.) :  Meteorological  Observations  made  at  Providence, 
R.  I.,  from  1831  to  1860.  Washington,  Smithsonian  Insti- 
tution, 1860.  4to. 

CATALOGUES:  And  price  lists  of  astronomical  instruments.  [A 
very  complete  collection  is  available,  the  separate  numbers 
of  which  are,  however,  not  catalogued.  A  valuable  series  of 
photographs  of  instruments  supplements  the  collection.] 

CELLERIER  (G-.):  Etude  numerique  des  Concours  de  compensa- 
tion de  Chronometres,  etc.  Geneva,  1887.  4to.  P. 

CELORIA  (G.):  Sugli  eclissi  solari  totali  del  3  Guigno,  1239,  e 
del  6  Ottobre,  1241.  Milan,  1876.  folio.  P. 

CHABERT  (J.  B.  de):  Voyage  en  1750  et  1751  dans  1'Amerique 
Septentrionale.  Paris,  1753.  4to. 

CHACORNAC  (J.):  See  Paris. 

CHALMERS  (T.):  Discourses  on  the  Christian  Revelation  viewed 
in  connection  with  Astronomy.  New  York,  n.  d.  8vo. 

CHAMBERS  (G.  F.):  A  Hand  Book  of  Descriptive  Astronomy. 
1  vol.  Oxford,  1877.  8vo.  Also,  Same.  4th  edition.  3 
vols.  1889-90.  8vo. 

:  See  SMYTH. 

CHAMBERS  (W.  and  R.):  Information  for  the  People.  2  vols. 
Philadelphia,  1854.  8vo. 

CHAMBERS:  See  Encyclopaedia. 

CHANDLER  (S.  C.):  On  the  Square  Bar  Micrometer.  Cambridge, 
1885.  4to.  P. 

and  RITCHIE  (J.):  Telegraphic  Transmission  of  Astro- 
nomical Data.  I,  II  (The  Phrase  Code).  Boston,  1883. 
8vo.  P. 


26*  Catalogue  of  the 


CHAPEL  HILL  (N.  C.)  (ELISHA  MITCHELL  Scientific  Society): 
Journal,  5th  year  (1888),  part  2;  6th  year,  part  1.  Raleigh. 
8vo.  P. 

CHAPIN  (F.  H.):  Mountaineering  in  Colorado.  Boston,  1889. 
8vo. 

CHAPIN  (G.  L.):  Power  as  applied  to  matter,  etc.  Chicago, 
1887.  8vo.  P. 

CHAPULTEPEC  (observatory):  Anuario  (1881-82-83),  bound  in  1 
vol.  Mexico.  16mo. 

:  See  ANGUIANO.     See  Tacubaya. 

[CHARLESTON]:  Views  of  prominent  places  in  Charleston,  illus- 
trating the  Effect  of  the  Earthquake  of  1886.  New  York, 
1886.  4to.  P. 

CHARLIER  (C.  V.  L.):  Om  integrationen  af  differential-ekva- 
tionerna  for  den  intermediara  banan.  Stockholm,  1885. 
8vo.  P, 

:  En  metod  att  foroka  konvergensen  hos  en  trigonometrisk 

serie.     Stockholm,  1886.     8vo.     P. 

:  Unter  suchungueber  die  allgemeinen  Jupiter-Stoerungen 

des  planeten  Thetis.     Stockholm,  1887.     4to.     P. 

:  Ueber  die  Andwendung  der  Sternphotographie  zur  Hellig- 

keits-messungen  der  Sterne.     Leipzig,  1889.     4to.     P. 

:  Ett  forsok  att  bestamma   ljusets  hastighet  ur  observa- 

tionerfaforanderligastjernor.     Stockholm,  1889.     8vo.    P. 

CHAUVENET  (W.):  Binomial  Theorem  and  Logarithms.  Phila- 
delphia, 1843.  8vo. 

:  A  Manual  of  Spherical  and  Practical  Astronomy.     Vols.. 

I,  II.     Philadelphia,  1863.     8vo. 

:  New  method  of  correcting  Lunar  Distances,  etc.     New 

York,  1868.     8vo. 

:  A  treatise  on  the  Method  of  Least  Squares.  Philadel- 
phia, 18*68.  8vo. 

CHEYNE  (C.  H.  H.):  An  elementary  treatise  on  the  planetary 
theory.  3d  edition.  London,  1883.  16mo. 

CHICAGO  (Astronomical  Society):  The  Solar  Eclipse  of  July 
29,  1878.  Chicago,  1878.  8vo.  P. 

:  Report  for  1880-1-2-3-4-5-6.    Chicago.    8vo.    P. 

CHITTENDEN  (R.  H.):  Studies  in  Astronomy.  Marshall.   8vo.   P. 


Lick  Observatory  Library.  27* 

CHRISTIANIA    (observatory):     Zonenbeobachtungen    -{-65°    to 
+70°,   von    FEARNLEY    und    GEELMUYDEN.      Christiania, 

1888.  4to. 

CHRISTIE   (W.  H.  M.):    Description  of  the  personal  equation 

machine  (at)  Greenwich.     London,  n.  d.     8vo.     P. 
:  Ten-year  Catalogue  of  4059  stars  for  1880.0.     London, 

1889.  4to. 

CHURCH  (A.  E.):  Elements  of  Descriptive  Geometry.     1   vol. 

text,  1  vol.  plates.     New  York,  1865.     4to. 
CIEL  ET  TERRE:    2d  series;  5th  year  beginning  March  1,  1889 

(current).     Brussels.     8vo. 
CINCINNATI   (observatory):  Inaugural  Report  of  the  Director, 

1868,  and  Report,  1869.     Cincinnati,  1869.     8vo.     P. 
:  Publications,  1,  2,  3,  4,  5,  6,  bound  in  1  vol.     Cincinnati, 

1876-82.     8vo. 

CLAIRAUT  (A.  C.):  Theorie  de  la  Lune.     Paris,  1765.     4to. 
[CLARK]:    Framed   photographic   portraits  of  ALVAN   CLARK, 

GEORGE  B.  CLARK,  and  ALVAN  G.  CLARK,  in  one  group. 
CLARKE  (F.  W.):  The  Constants  of  Nature.     Part  I.     Wash- 
ington, 1873.     8vo. 
:  Report    *     *    on  Chemistry  and  Physics.   Bulletins  M.S. 

Geol.  Survey,  in  1883-4  (1  vol.),  1884-5  (1  vol.),  1885-6 

(1  vol.).     Washington.     Svo.     P. 
CLEVELAND  (P.):  Meteorological  Observations,  Brunswick,  Me., 

1807-59.     Washington,    Smithsonian    Institution,    1867. 

4to.     P. 
CLERKE  (A.M.):  A  Southern  Observatory  (C.G.  H.);  from  The 

Contemporary  Review.     London,  1889.     Svo.     P. 

:  The  System  of  the  Stars.     London,  1890.     Svo. 

CLIFFORD  ( W.  K.) :  Elements  of  Dynamic;  Kinematic  I,'  II,  III, 

IV.     2  vols.     London,  1878  and  1887.     12mo. 
COFFIN  (J.  H.):  Winds  of  the  Northern  Hemisphere.     Wash- 
ington, Smithsonian  Institution,  1853.     4to.     P. 
COFFIN  ( J.  H.  C.) :  Suggestions  for  observing  the  total  eclipse  of 

the  Sun  on  August  7,  1869.     Washington,  1869.     Svo.     P. 
:  Reports  of  observations  of  the  Total  Eclipse  of  the  Sun, 

August  7-,  1869.     Washington,  [1877].     4to. 


28*  Catalogue  of  the 


COIMBRA    (observatory):    Meteorological   observations.     [Trans- 
ferred to  the  University  Library,  Berkeley.] 
[COMETS]  :  Bronze  comet  medal  of  the  Astronomical  Society  of 

the  Pacific.    [Presented  by  Hon.  J.  A.  DONOHOE.] 
COMMON  (A.  A.):  Enlarged  photograph  of  the  nebula  of  Orion 

(framed). 

(The)  COMPANION  TO  THE  ALMANAC:  For  1830,  for  1832.    Lon- 
don, s.  d.     32mo. 
COMSTOCK  (G.  C.):  Tables  of  Precessions  for  1880  in  R.  A.  and 

Dec.     Madison,  1883.     8vo.     P. 
:  Memoir  of  J.  C.  WATSON,  1838-80.     Washington,  1888. 

8vo.     P. 
CONDAMINE  (Ch.  M.  de  la):  Mesures  des  trois  premiers  degres 

du  meridien,  etc.  Paris,  1751.  4to. 
CONDORCET  (M.  T.  A.  N.  G-.):  See  Berlin. 
COOPER  (E.  J.):  Catalogue  of  Stars  near  the  ecliptic.  Vols. 

1,  2,  3,  4.     Bound  in  2  vols.     Dublin,  1851-56.     8vo. 
COPELAND  (R.)  and  BOERGEN  (C.):  Mittlere  Oerter  der  in  den 

Zonen  — 0°  und  — 1°  der  DM.  enthaltenen  Sterne.     Gottin- 
.    gen,  1869.     4to. 

:  See  Copernicus. 

COPENHAGEN  (R.  Danish  Acadejny  of  Sciences):  Oversigt,  etc., 

1885,  (1887-8).  Copenhagen.  8vo. 
COPERNICUS:  An  International  Journal  of  Astronomy,  edited 

by  R.  COPELAND  and  J.  L.  E.  DREYER.     Vols.  I,  II,  III, 

bound  in  1  vol.     Dublin,  1881-84.     4to. 
CORDOBA    (National   Observatory):    Resultados   I    (1879)    and 

Atlas;    V    (1874);  VI    (1875);    (IX,   X)    (1876-7);   XIV 

(Cat.  Gen.)  (1886).     Buenos  Aires.     4to. 
:  Annual  Report  for  1874.     Informes  presentados  al  Minis- 

terio,  etc.  (for)  1873  and  1875.     Buenos  Aires.     8vo.     P. 
CORDOBA  (Meteorological  office):  Anales  I  (1878);  II  (1881);  III 

(1882);  IV  (1884);  V  (1887).     Buenos  Aires.     4to. 
CORK  (observatory):  See  GRUBB. 
CORRESPONDENCE  ASTRONOMIQUE:  Vols.  1-15.     Genoa,  1818-26. 

8vo. 
COURTANVAUX  (F.  C.  le  T.):  Journal  du  Voyage  sur  la  Frigate 

VAurore,  etc.     Paris,  1768.     4to. 


Lick  Observatory  Library.  29* 

CRAIG  (T.) :  A  general  differential  equation  in  the  theory  of  the 

deformation  of  surfaces.     Philadelphia,  1879.     8vo.     P. 
:  The  motion  of  a  Solid  in    a   Fluid.     Baltimore,   1879. 

4to.     P. 
:  General  properties  of  the  equations  of  steady  motion. 

Washington,  1881.     4to.     P. 
CRELLE  (A.  L.):    Rechentafeln.    3d  edition,  by  C.  BREMIKER. 

Berlin,  1869.     4to. 
:  Journal  fur   die   reine   und    angewandte    Mathematik. 

Vols.  1  (1826)  to  15,  inclusive;  parts  of  Vols.  16  and  18; 

Vols.  20-68,  inclusive— 1826  to  1867.    [Loaned  to  the  L.  0. 

by  GEORGE  F.  BECKER,  Ph.D.]     Berlin.     4to. 
:*Vols.   (100,  101),    (102,  103),  (104,  105);   bound  in  3 

vols.     Berlin,  1886-89.     4to. 

— :  Also  Index,  Vols.  1-100, 1826  to  1887.     Berlin,  1887.  4to. 
CROSSLEY  (E.),  GLEDHILL  (G.),  WILSON  (G.  M.):  A  Handbook 

of  Double  Stars.     1  vol.     Also,  corrections,  notes  to  above, 

1  vol.     London,  1879-80.     8vo. 

CRUDEN  (A.):  A  Concordance  to  the  Holy  Scriptures.     Phila- 
delphia, 1830.     8vo. 
CULLEY  (R.  S.):  Handbook  of  Practical  Telegraphy.     London, 

1885.     8vo. 
D'ABBADIE  (A.):  Recherches  sur  la  Verticale.     Brussels,  1881. 

8vo.     P. 

D'AGELET  (J.  L.  P.):  See  GOULD. 
DAGUIN  (P.  A.) :  Traite  elementaire  de  Physique.   4  vols.    Paris, 

1878-9.     8vo. 
DARQUIER   (A.  de  P.):    Observations  Astronomiques   faites  a 

Toulouse.     Avignon,  1777.     4to. 
D'ARREST  (H.  L.):  Siderum  nebulosorum  observationes  Hav- 

nienses.     Copenhagen,  1867.     4to. 
DARWIN  (G.  H.):  Saturn's  Rings   (from  Harper's  Magazine). 

New  York,  1889.     8vo.     P. 
DAUDELIN(P. G.):  Sur  la  determination  geometrique des orbites 

Cometaires.     n.  p.,  n.  d.     4to.     P. 
DAVENPORT  (Academy  of  Natural  Sciences) :  Proceedings.    Vols. 

(2,  3,  4),  bound  in  1  vol.     1876-84.     n.  p.,  n.  d.     8vo. 


30*  Catalogue  of  the 


DAVIDSON  (G.):  Field  catalogue  of  983  Transit  Stars.  Wash- 
ington, 1874.  8vo.  P. 

:  The  Star  factors  ABC  (tables).  Washington,  1874. 

4to.  P. 

:  Description  of  an  improved  open  vertical  clamp,  etc. 

Washington,  1880.  4to.  P. 

:  Field  Catalogue  of  Time  and  Circumpolar  Stars  for  1885. 

Washington,  1884.  8vo.  P. 

:  The  Run  of  the  Micrometer.    Washington,  1885.    4to.    P. 

:  Photographed  copy  of  a  relief  map  of  California,  etc. 

:  The  Endowment  of  Scientific  Research.  San  Francisco, 

n.  d.  4to.  P. 

:  See  Washington  (U.  S.  Coast  Survey). 

and  SCHOTT  (C.  A.) :  Heights  of  the  Stations  of  the  DAVID- 
SON Quadrilaterals.  Washington,  1885.  4to.  P. 

DAVIES  (C.):  Elements  of  Surveying.  4th  edition.  Hartford, 
1839.  8vo. 

:  New  Elementary  Algebra,     n.  p.,  n.  d.     12mo. 

DAVIS  (C.  H.):  Law  of  Deposit  of  the  Flood  Tide.  Washing- 
ton, Smithsonian  Institution,  1851.  4to.  P. 

[ ]:   (Biography  of),     n.  p.,  n.  d.     8vo.     P. 

DAVIS  (W.  G.):  Ligeros  Apuntes  sobre  el  clima  de  la  Repub- 
lica  Argentine.  Buenos  Aires,  1889.  4to.  P. 

DELAMBRE  (J.  B.):  Histoire  de  1'astronomie  ancienne  (i,  ii), 
1817;  du  moyen  age,  1819;  moderne  (i,  ii),  1821;  au  XVIII 
siecle,  1827.  Paris,  1817-27.  4to. 

DE  LA  HIRE  (P.) :  Tabulae  Astronomicse,  etc.     Paris,  1727.     4to. 

DE  LA  RUE  (W.):  Comparison  of  DE  LA  RUE'S  and  SECCHI'S 
Eclipse  Photographs.  London,  1864.  8vo.  P. 

,  STEWART  (B.),  and  LOEWY  (B.):  Researches  in  Solar 

Physics,  2d  series — (areas  of  sun  spots).  London,  1866. 
4to.  P. 

:  Researches  in  Solar  Physics.  Appendix  to  second  series, 

etc.,  on  the  distribution  in  heliographic  latitude  of  the  Sun 
spots,  observed  by  CARRINGTON.  London,  1868.  4to.  P. 

DEMBOWSKI  (E.):  Misure  micrometrische  di  Stelle  doppie  e 
multiple  (1852-78).  2  vols.  Rome,  1883-84.  4to. 

[DE  MORGAN  (A.)]:  BARLOW'S  Tables  of  Squares,  Cubes,  etc. 
London,  1875.  8vo. 


Lick  Observatory  Library.  31* 

DENVER  (CHAMBERLIN  Observatory):  Publications  No.  1,  1889. 
4to.  P. 

DENZA  (F.):  Le  Stelle  Cadenti  del  period!  di  Agosto  e  di  No- 
vembre,  1887,  etc.,  also,  1888.  Turin,  1888-9.  16mo.  P. 

DESAINS  (M.  P.):  Logons  de  Physique.  Vols.  I,  II.  Paris, 
1857-60.  8vo. 

DESCHANEL  (A.  P.):  Traite  elementaire  de  Physique.  Paris, 
1869.  8vo. 

[DICTIONARY]:  NEUMAN  &  BABETTI'S  Dictionary  of  the  Span- 
ish and  English  Languages.  Vol.  II  (only),  English  and 
Spanish.  Boston,  1845.  Svo. 

[ ]:  A  Classical  Dictionary,  etc.,  by  C.  ANTHON.     New  York, 

1856.     Svo. 

[ ] :  Comprehensive  Dictionary  of  the  English  Language,  by 

J.  E.  WORCESTER.     Boston,  1876.     Svo. 

[ ]:    Dictionary   of    the   English    and    Dutch    Languages 

[TAUCHNITZ].     Leipzig,  1878.     32mo. 

[ ]:  SPIERS  &  SURENNE'S  French  and  English  Dictionary. 

New  York,  1880.     Svo. 

[ ] :  Dictionary  of  the  English  and  Italian  Languages,  by 

JAMES  &  GRASS:  [TAUCHNITZ].     Leipzig,  1882.     12mo. 

[ ]:  A  new  Dictionary  of  the  English  and  Danish  Lan- 
guages [TAUCHNITZ].  Leipzig,  1883.  32  mo. 

[ ]:  Dictionary  of  the  English   and   Swedish   Languages 

[TAUCHNITZ].     Leipzig,  1883.     32mo. 

[ ] :  Dictionnaire  de  la  langue  franchise     *     *     *     par  A. 

BEAUJEAN.     7th  edition.     Paris,  1883.     Svo. 

[ ] :  Dictionary  of  the  German  and  English  Languages,  by 

G.  J.  ADLER.     New  York,  1884.     Svo. 

'[ ]:  The  Imperial  Dictionary.    4  vols.  complete.    New  York, 

1885.     Svo. 

[ ]:  (Pocket)  Dictionary  of  the  Latin  and  English  Lan- 
guages [TAUCHNITZ].  Leipzig,  1886.  32mo. 

[ ]:  THIEME-PREUSSER;  German-English  Dictionary.  Ham- 
burg, 11.  d.  Svo. 

DOBERCK  (W.):  On  Omega  Leonis  considered  as  a  revolving 
double  star.  Dublin,  1876.  4to.  P. 

:  Markree  Observatory.     London,  1884.     Svo.     P. 

:  The  Inventor  of  the  Telescope.     London,  n.  d.    Svo.     P. 


32*  Catalogue  of  the 


DOELLEN  (W.):  Zeitsterne-Ephemeriden  auf  das  Jahr  1886-87- 

88-89-90.     5  vols.     St.  Petersburg,  1886-88.     8vo.     P. 
DOLGOUROUKI:   [On  the  Secular  acceleration  of  the  Moon's  mean 

motion];  in  Russian.     St.  Petersburg,  1885.     8vo.     P. 
DONNER  (A.):    Beobachtungen  von  Cometen,  1885-86.     1  vol. 

Helsingfors,  1889.     4to.     P. 
DORPAT  (observatory):  Observations  astronomicse  (W. STRUVE). 

Vol.  I- VIII,  pro  annis  1813-38.      Dorpat,  1817-39.     4to. 

Beobachtungen  (J.  H.  MAEDLER),  bd.  9,  10,  11,  12,  13,  14, 

15,  16.     1841-66.     Dorpat,  1842-66.     4to. 

:  (L.  SCHWARZ),  bd.  17,  18,  20.     Dorpat,  1887-91.     4to. 

[These  works  have  been  kindly  presented  to  the  L.  0.,  but  have  not 

arrived  at  the  time  of  printing  this.] 

DOWNING  (A.  M.  W.):  On  the  orbit  of  Gamma  Coronas  Australis. 

London,  1883.     8vo.     P. 
:  On  an  instance  of  change  of  personality  in  observing 

position  angles  of  double  stars;  and  on  the  orbit  of  Alpha 

Centauri.     London,  1884.     8vo.     P. 
:  Discussion  of  the  observations  of  the  Sun  made  with  the 

Washington  Transit  Circle,  1875-83.  London,  1889.  8vo.  P. 
:  Probable  Errors  of  Greenwich  determinations  of  R.  A.  at 

different  Z.  D.     London,  1889.     8vo.     P. 

DRAPER  (H.) :  Large  Photograph  of  the  Moon,  September  3, 1863. 
:  On  the  Construction  of  a  Silvered  Glass  Telescope.  Wash- 
ington, 1864.     4to.     P. 
:  On  the  Construction  of  a  Silvered  Glass  Telescope  [bound 

with  other  memoirs].     Washington,  1864.     4to. 
:  Photographs  of  the  Spectra  of  Venus  and  Alpha  Lyrse. 

New  Haven,  1877.     8vo.     P. 
[ ] :  Bronze  Replica  of  the  Obverse  of  the  HENRY  DRAPER 

medal  of  the  National  Academy  of  Sciences.   [Presented  by 

Mrs.  DRAPER.] 

[ ]:  Framed  photographic  portrait  of  HENRY  DRAPER. 

DRAPER  ( J. W. ) :  Science  in  America.   New  York,  1876.   16mo.  P. 

:  On  a  new  form  of  Spectrometer.  New  Haven,  1879.  8vo.  P. 

:  Scientific  Memoirs.     New  York,  1878.     8vo. 

[ ]:  Memoir  of,  by  G.  F.  BARKER,     s.  L,  s.  d.  [1866]. 

[ ] :  Large  portrait  of  j .  W.  DRAPER. 

DRESDEN  (observatory):  Observations  astronomiques  faites  par 

B.  d'ENGELHARDT,  etc.     Part  I.     Dresden,  1886.     4to. 


Lick  Observatory  Library.  33* 

DREYER  (J.    L.  E.):   A  record  of  the  progress  of  Astronomy 

during  1879.     Dublin,  1880.     8vo.     P. 
:  Note  on  the  Meteors  Connected  with  the  first  Comet  of 

1860.     Dublin,  1880.     8vo.     P. 

:  The  instruments  in  the  old  observatory  at  Peking.    Dub- 
lin, 1881.     8vo.     P. 
:  A   new  determination  of  the    Constant  of   Precession. 

Dublin,  1882.     8vo.     P. 
:  On  the  proper  motion  of  twenty-nine  telescopic  stars. 

London,  1886.     8vo.     P. 
:  On  some  nebulae  hitherto    suspected  of   variability  or 

proper  motion.      Note  on  the  effect  of  refraction  in  Stellar 

photography.     London,  1887.     8vo.     P. 
:  On  the  multiple  tail  of  the  great  Comet  of  1744.     n.  p., 

n.  d.     4to.     P. 
:   (The)  Article  "  Observatory,"  from  Encyclopaedia  Britan- 

nica  (1884).     n.  p.,  n.  d.     4to.     P. 
:  Observation  of  the  Transit  of  Venus,  1882.      Dublin, 

n.  d.     8vo.     P. 

:  TYCHO  BRAKE.     Edinburgh,  1890.     8vo. 

:  See  ARMAGH.     See  COPERNICUS. 

DUBLIN  (Royal  Dublin  Society):   Scientific  Transactions  (new 

series).     Dublin,  1877-89.     4to. 

Contents:  Vol.  I.  1.  On  Great  Telescopes  of  the  Future.  By  HOWARD 
GRUBB.  (November,  1877.)  — 2.  On  the  Penetration  of  Heat  across 
Layers  of  Gas.  By  G.  J.  STONEY.  (November,  1877.)  —  3.  On  the  Satel- 
lites of  Mars.  By  WENTWORTH  ERCK.  (May,  1878.)  —  4.  On  the  Mechanical 
Theory  of  CROOKES'S,  or  Polarization  Stress  in  Gases.  By  G.  J.  STONEY. 
(October,  1878.)  —  5.  On  the  Mechanical  Theory  of  CROOKES'S  Force.  By 
GEORGE  FRANCIS  FITZGERALD.  (October,  1878.)  —  6.  Notes  on  the  Phys- 
ical Appearance  of  the  Planet  Mars,  as  seen  with  the  3-foot  Reflector  at 
Parsonstown,  during  the  Opposition  of  1877.  By  JOHN  L.  E.  DREYER. 
With  Plates  I  and  II.  (November,  1878.)  —  *7.  On  the  Nature  and  Origin 
of  the  Beds  of  Chert,  etc.  By  Professor  EDWARD  HULL.  On  the  Chem- 
ical Composition  of  Chert,  etc.  By  EDWARD  T.  HARDMAN.  (November, 
1878.)  —  8.  On  the  Superficial  Tension  of  Fluids  and  its  Possible  Relation 
to  Muscular  Contractions.  By  G.  F.  FITZGERALD.  (December,  1878.)  —  9. 
Places  of  One  Thousand  Stars  observed  at  the  Armagh  Observatory.  By 
REV.  THOMAS  ROMNEY  ROBINSON.  (February,  1879.)  —  10.  On  the  Pos- 
sibility of  Originating  Wave  Disturbances  in  the  Ether  by  Means  of 
Electric  Forces.  By  GEORGE  FRANCIS  FITZGERALD.  (February,  1880.) 
—  *11.  On  the  Relations  of  the  *  *  *  Rocks  of  the  South  of  Ireland 
to  those  of  North  Devon.  By  EDWARD  HULL.  (May,  1880.)  —  12.  Phys- 
ical Observations  of  Mars,  1879-80.  By  C.  E.  BURTON.  With  Plates  VI, 
VII,  and  VIII.  (May,  1880.)  — 13.  On  the  Possibility  of  originating 


34*  Catalogue  of  the 


DUBLIN  (Royal  Dublin  Society):  Scientific  Transactions. 

Wave  Disturbances  in  the  Ether  by  means  of  Electric  Forces.  PART  2. 
By  GEORGE  FRANCIS  FITZGERALD.  (November,  1880.)  —  *14.  Explora- 
tions in  the  Bone  Cave  of  Ballynamintra.  By  A.  LEITH  ADAMS,  G.  H. 
KTNAHAN,  and  R.  J.  USSHER.  (April,  1881.)— 15.  Notes  on  the  Phys- 
ical Appearance  of  the  Planet  Jupiter  during  the  Season  1880-1.  By  the 
EARL  OF  ROSSE  and  Dr.  OTTO  BOEDDICKER.  Plate  XV.  (January,  1882.) 
— 16.  Photographs  of  the  Spark  Spectra  of  Twenty-one  Elementary 
Substances.  By  W.  A.  HARTLY.  Plates  XVI,  XVII,  and  XVIII.  (Feb- 
ruary, 1882.)  —  17.  Notes  on  the  Physical  Appearance  of  the  Comets  b 
and  c,  1881,  as  observed  at  Birr  Castle,  Parsonstown,  Ireland.  By  the 
EARL  OF  ROSSE  and  OTTO  BOEDDICKER.  Plate  XIX.  (August,  1882.)  — 
*18.  On  the  Laureiitian  Rocks  of  Donegal,  etc.  By  EDWARD  HULL. 
(February,  1882.)  —  19.  Paleeo-Geological  and  Geographical  Maps  of  the 
British  Islands  and  the  adjoining  parts  of  the  Continent  of  Europe. 
By  EDWARD  HULL.  Plates  XXII  to  XXV.  (November,  1882.)  — 20. 
Notes  on  the  Physical  Appearance  of  the  Planet  Mars  during  the  Oppo- 
sition in  1881.  Accompanied  by  Sketches  made  at  the  Observatory, 
Birr  Castle.  By  OTTO  BOEDDICKER.  Plates  XXXVI  and  XXXVII. 
(December,  1882.)  —  21.  Notes  on  the  Aspect  of  Mars  in  1882.  By  C.  E. 
BURTON.  As  seen  with  a  Reflecting  Telescope  of  9-inch  Aperture,  and 
Powers  of  270  and  600.  Plate  XXXVIII.  (January,  1883.)  —  22.  On  the 
Energy  expended  in  Propelling  a  Bicycle.  By  G.  JOHNSTONE  STONEY 
and  G.  GERALD  STONEY.  Plates  XXXIX,  XL,  and  XLI.  (January, 
1883.)  —  23.  On  Electromagnetic  Effects  due  to  the  Motion  of  the  Earth. 
By  GEORGE  FRANCIS  FITZGERALD,  Erasmus  Smith's  Professor  of  Experi- 
mental Science  in  the  University  of  Dublin.  (January,  1883.)  —  24.  On 
the  Possibility  of  Originating  Wave  Disturbances  in  the  Ether  by  Means 
of  Electric  Forces— Corrections  and  Additions.  By  GEORGFE  FRANCIS 
FITZGERALD.  (January,  1883.)  —  *25.  On  the  Fossil  Fishes  of  the  Carbo- 
niferous Limestone  Series  of  Great  Britain.  By  J.  W.  DAVIS.  (Septem- 
ber, 1883.) 

Vol.  II.  1.  Observations  of  Nebulae  and  Clusters  of  Stars,  made  with 
the  6-foot  and  3-foot  Reflectors  at  Birr  Castle,  from  the  year  1848  up  to 
the  year  1878.  Nos.  1  and  2.  By  the  EARL  OF  ROSSE.  Plates  I  to  IV. 
(August,  1879.)  No.  3.  Plates  V  and  VI.  (June,  1880.)  —  2.  On  Aquatic 
Carnivorous  Coleoptera  or  Dytiscidse.  By  DR.  SHARP.  (April,  1882.)  4 

Vol.  III.  1.  On  the  Influence  of  Magnetism  on  the  Rate  of  a  Chro- 
nometer. By  OTTO  BOEDDICKER.  Plate  I.  (September,  1883.)  —  2.  On 
the  Quantity  of  Energy  transferred  to  the  Ether  by  a  Variable  Current. 
By  GEORGE  F.  FITZGERALD.  (March,  1884.)  —  3.  On  a  New  Form  of 
r  Equatorial  Telescope.  By  HOWARD  GRUBB.  Plate  II.  (March,  1884.) 
—  *4.  Catalogue  of  Vertebrate  Fossils  from  the  Siwaliks  of  India,  etc. 
By  R.  LYDEKKER.  (July,  1884.)  —  *5.  On  the  Origin  of  Freshwater 
Faunas.  By  W.  J.  SOLLAS.  (November,  1884.)  —  *6.  Memoirs  on  the 
Coleoptera  of  the  Hawaiian  Islands.  By  the  REV.  T.  BLACKBURN  and 
DR.  D.  SHARP.  (February,  1885.)  —  7.  Notes  on  the  Aspect  of  the  Planet 
Mars  in  1884.  Accompanied  by  Sketches  made  at  the  Observatory,  Birr 
Castle.  By  OTTO  BOEDDICKER.  Plate  VI.  (March,  1885.)  —  *8.  On  the 
Geological  Age  of  the  North  Atlantic  Ocean.  By  EDWARD  HULL. 
(April,  1885.)  — 9.  On  the  Changes  of  the  Radiation  of  Heat  from  the 
Moon  during  the  Total  Eclipse  of  1884,  October  fourth,  as  Measured  at 
the  Observatory,  Birr  Castle.  By  OTTO  BOEDDICKER.  Plates  IX  and  X. 


Lick  Observatory  Library.  35* 

DUBLIN  (Royal  Dublin  Society):  Scientific  Transactions. 

(October,  1885.)  —  *10..0n  the  Collection  of  the  Fossil  Mammalia  of  Ire- 
land, etc.  By  V.  BALL.  (November,  1885.)  —  *11.  On  New  Zealand 
Coleoptera.  By  DAVID  SHARP.  (November,  1886.)  —  *12.  The  Fossil 
Fishes  of  the  Chalk  of  Mount  Lebanon.  By  JAMES  W.  DAVIS.  (April, 
1887.)  — 13.  On  the  Cause  of  Iridescense  in  Clouds.  By  G.  JOHNSTONE 
STONEY.  (May,  1887.)  —  *14.  The  Echinoderrn  Fauna  of  the  Island  of 
Ceylon.  By  F.  JEFFRY  BELL.  (November,  1887.) 

Also:  Vol.  IV  (Parts  1-5). 

[The  above  bound  in  one  volume;  the  papers  marked  *  transferred  to 
the  general  library  of  the  University  of  California  before  binding.] 

:  Scientific  Proceedings.     Vols.  1,  2,  3,  4,  5,  6  (complete). 

Dublin,  1877-90.     8vo. 
DUBLIN  (Royal  Irish  Academy):   Transactions;  Vol.26,  parts 

1,  3,  4,  7,  10,  11,  16;  Vol.  29,  part  13.     Proceedings,  third 

series,  Vol.  I  (1888^90).     Cunningham  Memoirs;  III,  IV. 

Dublin.     4to  and  8vo. 
DUFOUR  (C.):    Sur  une  nouvelle  methode  pour  determiner  la 

distance  de  quelques  etoiles.     Geneva,  1868.     8vo.     P. 
DUHAMEL    (J.    B.):    Regise   Scientiarum   Academise    Historia. 

Paris,  1701.     4to. 
DUN  ECHT  (Lord  Crawford's  Observatory):   Publications;  Vols. 

I  (1876),  II  (1877),  III  (1885).     Dun  Echt.     4to. 
DUNER  (N.  C.):  Sur  les  etoiles  a  spectres  de  la  troisieme  classe. 

Stockholm,  1884.     4to. 

:  Sur  la  rotation  du  Soleil.     Stockholm,  1890.     8vo.     P. 

and  ENGSTROM  (F.):  Observations  des  etoiles  de  la  Zone 

+35°,  +40°,  faites  a  Pobservatoire  de  Lund  et  reduites  a 

1875.0.     Vol.  II,  parts  1  and  2.     Lund,  1889.     4to.     P. 
DUNSINK  (University  Observatory):  Astronomical  Observations 

and  Researches;  I,  II,  III  (1870-79);  IV,  V  (1882-84).     2 

vols.     Dublin.     4to. 
DURER  (A.)  and  OTHERS:  I.  Imagines  Coeli  Meridionales.     II. 

Imagines  Coeli  Septentrionales  cum  duodecim  imaginibus 

Zodiaci.     IOANN  STABIUS  ordinauit,  CONRADUS  HEINFOGEL 

Stellas  posuit,  ALBERTUS  DURER  imaginibus  circumscripsit. 

[Two  maps,  presented  by  Dr.  C.  H.  F.  PETERS.]     Vienna, 

1515.     folio. 
EASTMAN  (J.  R.):  November  meteors  of  1868.      Washington, 

1868.     8vo.     P. 


36*  Catalogue  of  the 


EASTMAN  (J.  R.):  Tables  of  the  Instrumental  Constants,  etc., 

for  the  reduction  of  Transit  Observations,  etc.  (Wash.  Ast. 

Obs.  for  1872).     Washington,  1873.     4to. 
:  Internal   contacts   in   transits  of   the   inferior   planets. 

Salem,  1883.     8vo.     P. 
:  Assumption  and  fact  in  the  theories  of  solar  and  stellar 

proper  motions.     Washington,  1889.     8vo.     P. 
EBERT  (H.):  Ueber  die  Abhaengigkeit  der  Wellenlaenge  des 

Lichtes  von  seiner  Intensitaet.     n.  p.,  1887.     8vo.     P. 
:  Die  Methode  der  Hohen  Interferenzen,  etc.     n.  p.,  1888. 

8vo.     P. 
:  Die  Methode  der  Hohen  Interferenzerscheinungen,  etc. 

Leipzig,  1888.     8vo.     P. 
:  Ueber  den  Einfluss  der  Dicke  und  Helligkeit  der  strah- 

lenden  Schicht  auf  das  Aussehen  des  Spectrums.     n.  p., 

1888.     8vo.     P. 
:  Ueber  den  Einfluss  der  Schwellenwerthe  der  Lichtemp- 

findungauf  den  Charakter  der  Spektra.    n.  p. ,1888.  8vo.  P. 

:  Optische  Mittheilungen.     Erlangen,  1889.     8vo.     P. 

:  See  WIEDEMANN. 

EDINBURGH   (Royal   Observatory):    Astronomical   Observations. 

Vols.  (2-3)"(1836-37);  (4-5-6)    (1838-40);    7  (1841);  8 

(1842);  9(1843);  10(1844-7);  11(1849-54);  15(1877-86). 

Edinburgh.     4to. 
EDINBURGH  (Royal  Society):  Proceedings.     10  (1878-80);    11- 

12-13-14-.     Edinburgh.     8vo. 

:  List  of  Members.     Edinburgh.     4to.     P. 

ELGER  (T.  G-.):  Physical  Observations  of  Saturn  in  1887 — in 

1888.     London,  1887-88.     8vo.     P. 
ELKIN  (W.  L.):  Ms.  list  of  stars  having  a  proper  motion  greater 

than  0".4.     Lick  Observatory,  1889.     4to.     P. 
ELLERY  (R.  J.  L.),  TODD  (C.),  and  RUSSELL  (H. C.):  Report  on 

the  telegraphic   determination  of  Australian  longitudes. 

Melbourne,  1886.    4to.     P. 
EMORY   (W.  H.):    Report  on   the     *     *     Mexican  Boundary 

Survey.     Vol.  I.     Washington,  1857.     4to. 
ENCKE  (J.  F.):  De  Formulis  Dioptricis.     Berlin  (1844).     4to. 
:  Sur  la  difference  des  longitudes  entre  Berlin  et  Bruxelles, 

etc.     Brussels,  n.  d.     8vo.     P. 
[ ] :  Life  of.     See  BRUHNS. 


Lick  Observatory  Library.  37* 

ENCYCLOPEDIA  METROPOLITANA:  Vol.11  (mixed  Sciences).  Lon- 
don, 1830.  4to.  ' 

[ENCYCLOPAEDIA]:  The  Penny  Cyclopaedia.  Vols.  1-27  (com- 
plete). London,  1833-43.  8vo. 

[ENCYCLOPEDIA  AMERICANA]:  1 3  vols.  (complete).  Philadelphia, 
1842.  8vo. 

[ENCYCLOPEDIA]:  Iconographic  Encyclopedia.  4  vols.  text,  2 
vols.  plates.  New  York,  1852.  4to. 

[ ] :  APPLETON'S  Cyclopaedia  of  Drawing,  by  W.  E.  WORTHEN. 

New  York,  1857.  8vo. 

[ENCYCLOPEDIA  BRITANNICA]  :  Vols.  1  to  24,  with  Vol.  25,  Index. 
American  Supplement,  Vols.  1,  2,  3.  New  York,  1878-87. 
4to. 

[  ENCYCLOPEDIA]  :  CHAMBERS'  Encyclopedia,  10  vols.  (complete). 

Philadelphia,  1860-68.     8vo. 

:  Same,  new  edition,  Vol.  II  (only).  Edinburgh,  1888.  8vo. 

ENGELHARDT  (B.  von).     See  Dresden. 

ENGELMANN  (R.):  Resultate  aus  Beobachtungen  auf  der  Leip- 

ziger  Sternwarte,  I.     Beobachtungen  am  Meridian  Kreis. 

Leipzig,  1870.     4to. 
:  Populare  Astronomic  von  SIM.  NEWCOMB.    Leipzig,  1881. 

8vo. 
:  Doppelsternmessungen  (from  Ast.  Nach.,  Vols.  115,  117). 

Kiel.     4to.     P. 

:  See  BESSEL.     See  Leipzig  Observatory.     See  NEWCOMB. 

ENGINEERING:  Vols.  46  (1888);  47  (1889);  48  (1889);  49  (cur- 
rent).    London,     folio. 
(The)  ENGLISH  MECHANIC:  Vol.  9,  10,  12,  13,  14,  15,  16, 17, 18, 

19,  20,  21,  22,  23,  24,  25,  26,  27,  28,  29,  30,  31,  32,  33,  34. 

[Temporarily  loaned  to  the  L.  0.   by   S.  W.  BURNHAM.] 

London,  1869-82.     Svo. 
ENGSTROM  (F.):    Bestamning  af  Lunds   Observatorii  Polhojd. 

Lund,  1889.     4to.     P. 

:  See  DUNER. 

ENNIS  (J.):  [Ten   pamphlets  011  the  nebular  hypothesis  and 

allied  subjects],  bound  in  1  vol.     1872-83.     8vo. 
ERICSSON  (G.):    Bestamning  af  Upsala  Observatorii   Polhojd. 

Upsala,  1885.     Svo.     P. 


38*  Catalogue  of  the 


ERICSSON  (G-.):  Definitive  Bahnelemente  des  Cometen  1863, 
III.  Upsala,  1888.  8vo.  P. 

ESPIN  (T.  E.):  A   Catalogue  of  the  magnitudes   of  500  stars 
*     *     *     from  photographs.     Liverpool,  1884.     8vo.     P. 

:  Photographic  Photometry,  etc.     Liverpool,  1887.    Svo.  P. 

ESTES  (L.):  Latitude  of  the  Detroit  Observatory  (of)  Ann 
Arbor.  Ann  Arbor,  1888.  Svo.  P. 

EULER  (L.):  Novse  Tabulae  Lunares.  St.  Petersburg,  1772. 
Svo. 

EVERETT  (E.):  Correspondence  relative  to  the  award  of  the 
King  of  Denmark's  Comet  medal  to  Miss  MITCHELL,  etc. 
(1847.)  Cambridge,  1849,  Svo.  P. 

EVERETT  (J.  D.):  Units  and  Physical  Constants.  London, 
1879.  12mo. 

:  (Secretary):  XV  Report  of  the  Committee  on  Under- 
ground Temperature,  B.  A.  A.  S.  London,  n.  d.  Svo.  P. 

EWING  (J.  A.):  Earthquake  measurement.    Tokio,  1883.   4to.  P.. 

:  Earthquakes  and  how  to  measure  them.     London,  18S8. 

Svo.    P. 

:  Seismometric  measurements  of  the  vibration  of  the  new 

Tay  bridge.     London,  1888.     Svo.     P. 

FABRY  (L.  de):  *  *  *  Le  premier  principe  du  calcul  dif- 
ferentiel.  Paris,  1866.  Svo.  P. 

FARADAY  (M.):  Experimental  Researches  in  Electricity.  Vols. 
I,  II,  III.  London,  1839-55.  Svo. 

FAYE  (H.  A.  E.  A.):    Remarques  au  sujet  des  recentes  experi- 
ences de  M.  HIRN  sur  la  vitesse  d'ecoulement  des  gaz.  Paris,  • 
1885.     4to.     P. 

FEARNLEY  (C.):  Venuspassagen  d.  6  December,  1882.  Christi- 
ania,  1883.  P. 

:  See  Christiania. 

FEDORENKO  (L):  Etoiles  circompolaires  dont  les  observations 
ont  ete  publiees  par  LALANDE.  St.  Petersburg,  1854.  4to. 

FEIL  ( )  and  FREMY  ( ):  On  the  artificial  production  of 

minerals  and  precious  stones.     Dublin,  1878.     Svo.     P. 

FERREL  (W.):  Tidal  Researches.     Washington,  1874.     4to. 

FERRERS  (N.  M.):  An  elementary  treatise  on  Spherical  Har- 
monics. London,  1877.  12mo. 


Lick  Observatory  Library.  39* 

FIGEE  (S.)  and  ONNEN  (H.):  Uitbarstingen  van  Vulkanen  en 
Aard  bevingen  in.  den  0.  I.  Archipel  waargenomen  ged- 
urende  het  Jaar  1884-85-86-87-88-89.  (Bound  in  one 
vol.)  (Batavia.)  8vo. 

FINLAY  (W. H.):  Observations  [and  Elements]  of  Comet  1884 
(BAENARD).  London,  1884.  8vo.  P. 

FISHER  (G.  P.):  See  SILLIMAN. 

FITZROY  (Admiral):  The  Weather-Book.     London,  1863.     8vo. 

FLAMMARION  (C.):  Catalogue  des  Etoiles  Doubles  et  Multiples. 
Paris,  1878.  Svo. 

FLAMSTEED  (J.):  Histories  Coelestis  Britannica?.  3  vols.  Lon- 
don, 1725.  folio. 

:  Atlas  Coelestis.     London,  1729.     folio. 

:  See  BAILY. 

FLINT  (A.  S.):  On  the  most  probable  value  of  the  latitude 
*  *  *  (in)  TALCOTT'S  method.  (Charlottesville),  1887. 
Svo.  P. 

:  A  brief  control  for  general  solutions  of  normal  equations. 

n.  p.,  1888.  Svo.  P. 

FOERSTER  ( W.) :  Sammlung  von  Hiilfstafeln  der  Berliner  Stern- 
warte.  Berlin,  1869.  4to. 

:  Sammlung  populaerer  astronomischer  Mittheilungen. 

Berlin,  1884.  Svo.  P. 

:  See  BRUHNS. 

FOLIE  (F.):  Sur  la  nutation  seculaire  de  1'axe  du  monde,  etc. 
Brussels,  1886.  12mo.  P. 

FORBES  (A.):  California.     London,  1839.     Svo. 

FORCE  (P.):  Auroral  Phenomena  in  North  Latitudes.  Wash- 
ington, Smithsonian  Institution,  [1856].  4to.  P. 

FOREL  (F.  A.):  Les  tremblements  de  terre  (en  suisse),  1880, 
1881,  (1882-3),  (1884-85-86).  4  numbers.  Geneva. 
Svo.  P. 

FONTENELLE  (B.  C.  B.):  Elemens  de  la  Geometric  de  1'infini. 
Paris,  1727.  4to. 

FRANZ  (J.):  Ueber  die  astronomischen  Beobachtungen  des 
Mondes.  Koenigsberg,  1889.  4to.  P. 

FREMONT  (J.  C.):  Report  of  the  Exploring  Expedition  to  the 

Rocky  Mountains  in    *     *    1842.  Washington,  1845.    Svo. 
11 


40*  Catalogue  of  the 


FRTTSCHE  (H.):  Untersuchungen  ueber  den  Doppelstern  STRUVE 

3121.     St.  Petersburg,  1866.     8vo.     P. 
FUCHS  (C.  W.  C.):  Statistik  der  Erdbeben,  1865-85.     Vienna, 

1886.     Svo. 
FUNK  (C.):  1.  *     *     *     Kosmogonie.      2.  Nachtrag.      Helm- 

stedt,  1888  and  1889.     Svo.     P. 
Fuss  (V.):  Ueber  die  Astronomische  Strahlenbrechung  in  der 

Nahe  des  Horizontes.     St.  Petersburg,  1872.     folio. 
G-ALLE  (J.  G.):  Ueber  eine  Bestimmung  der.Sonnen  Parallaxe 

aus    Beobachtungen  des  Planeten   Flora.     Breslau,  1875. 

Svo.     P. 
:  Variation  der  magnetischen  deklination  (in)    Breslau. 

Breslau,  n.  d.     4to.     P. 
GALLE  (A.):  Zur  berechnung  der  proximitaten  von  Asteroiden- 

bahnen.     Breslau,  1883.     Svo.     P. 

GANNETT  (H.):  List  of  elevations  in  the  U.  S.  west  of  the  Miss- 
issippi.    3d  edition.     Washington,  1875.     Svo.     P. 

:  Approximate  areas  of  the  U.  S.,  the  several  States,  etc. 

^Washington,  1881.     4to.     P. 

:  A   Dictionary   of  Altitudes   in  the  U.  S.     Washington, 

1884.     Svo.  .P. 
:    Boundaries  of  the  U.  S.  and  of  the  several  States,  etc. 

Washington,  1885.     Svo.     P. 

GARTZ  (J.  Ch.):  HERSCHEL  (Sir  W.).     n.  p.,  n.  d.     4to.     P. 
GAUSS  (C.  F.)  and  SCHUMACHER  (H.  C.):  Briefwechsel.     Vols. 

l_2_3_4-(5,  6).     Altona,  1860.     Svo. 

:   Werke.     7  vols.     Gottingen,  Gotha,  1863-74.     4to. 

and  BESSEL  (F.  W.):  Briefwechsel.     Leipzig,  1880.     Svo. 

GAUSS   (F.  G.):    Fiinfstellige     *     *     *      logarithmische   und 

trigonometrische  Tafeln.     Halle,  1885.     Svo. 
GAUTIER  (E.):    Notice   historique,  etc.,  sur  1'observatoire   de 

Geneve.     Geneva,  1883.     Svo.     P. 
:  Onzieme  Assemblee  generale  de  la  Societe  Astronomique 

(Ast.  Gesell.).     Geneva,  1885.     Svo.     P. 
:  Rapport  sur  le  concours  pour  le  reglage  des  Chronom- 

etres,  1887.     Geneva,  18S8.     Svo.     P. 
GEELMUYDEN  (H.):  See  Christiania. 
GENEVA  (observatory):  See  GAUTIER. 


Lick  Observatory  Library.  41* 

GEORGETOWN  (College  Observatory) :  Annals,  No.  1.     New  York, 

1852.     4to. 
GERNERTH  (A.):  Funstellige  Gemeine  Logarithmen  der  Zahlen 

imd  der  Winkelfunctionen  von  10  zu  10  secunden.    Vienna, 

1866.     8vo. 

GESELLSCHAFT  URANIA:  See  Berlin.     See  Himmel  und  Erde. 
GIBBS  (J.  W.):  On  multiple  algebra.    Salem,  1886.    8vo.    P. 
GIBBS  (W.):  On  the  construction  of  a  normal  map  of  the  Solar 

Spectrum.     New  Haven,  1867.     8vo.     P. 

GIHON   (J.  L.):  The  Photographic  Colorists  Guide.     Philadel- 
phia, 1878.     Svo. 
GILBERT  (G.  K.):  A  new  method  of  measuring  heights  by  the 

barometer.     Washington,  1882.     Svo.     P. 

:  Special  processes  of  research.    New  Haven,  1886.   Svo.    P. 

GILBERT  (L.  W.):  Annalen  der  Physik;  Vols.  1-76,  inclusive, 

with  Index,  1799-1824.     [Loaned  to  the  L.  0.  by  GEORGE 

F.  BECKER,  Ph.D.]     76  vols.     Halle-Leipzig.     Svo. 
GILL  (D.):  Cape  Catalogue  of  4810  Stars  for  1850.     n.p.,  n.  d. 

Svo. 
GILLISS   (J.  M.):  The  U.  S.  Astronomical  Expedition  to   the 

Southern   Hemisphere.      Vol.   I,    Vol.   II.      Washington, 

1855.     4to. 
:  An  account  of  the  total  eclipse  of  the  Sun,  September  7, 

1858.     Washington,  1859.     4to.     P. 
:  A   catalogue  of  1963    (southern)    Stars.      Washington, 

1870.     4to. 

GLASENAPP  (S.):  Satellites  of  Jupiter  (in  Russian).     St.  Peters- 
burg, 1874.     Svo. 
:  [On  Stellar  Parallaxes]   (in  Russian).     St.  Petersburg, 

1881.     Svo.     P. 

:   [On  Comets]  (in  Russian).    St.  Petersburg,  1881.   Svo.   P. 

:  Orbit  of  the  binary  Star  Lambda    Ophmchi.     London, 

1888.     Svo.     P. 
:  Total  Solar  Eclipse,  1887,  August  18  (in  Russian).     St. 

Petersburg,  1888.     4to.     P. 
:  Orbites  des  etoiles  doubles  du  Catalogue  de  Poulkova. 

St.  Petersburg,  1889.     Svo.     P. 
GLASGOW  (Scotland)  (observatory):  See  GRANT. 


42*  Catalogue  of  the 


GLASGOW    (U.   S.)    (MORRISON   Observatory):    Publications   of 

the  MORRISON  Observatory  No.  1.     Lynn,  1887.     4to. 
GLAZEBROOK  (R.  T.)  and   SHAW   (W.  N.):  Practical   Physics. 

2d  edition.     London,  1886.     12mo. 
GLEDHILL  (J.):  Measures  of  484  Double  Stars.     London,  n.  d. 

4to.     P. 

:  See  CROSSLEY. 

GODFRAY  (H.):  An  Elementary  Treatise  on  the  Lunar  Theory. 

Cambridge,  1859.     8vo. 
GODWARD  (W.):  Auxiliary  Tables  for  Computing  an  ephemeris 

of  a  minor  planet,  etc.     London,  1866.     4to. 
GOENS   (D.    van):     Disputatio    philosophica,    comprehendens 

Examen,  An  Luna  Habitabilis  Sit.     Cologne,  1738.   4to. 
GOTTINGEN  (observatory):  Astronomische  Mittheilungen,  Erster 

Theil.     Gottingen,  1869.     4to. 
(observatory):    Veroeffentlichungen,  Nos.  1,  2,  3,  4.     1  vol. 

Gottingen,  1878.     8vo.     P. 

:  See  COPELAND  and  BORGEN. 

GOODE  (G.  B.):  The  beginnings  of  Natural  History  in  America. 

Washington,  1886.     8vo.     P. 

:  The  beginnings  of  American  Science.     The  Third  Cen- 
tury.    Washington,  1888.     8vo.     P. 
GORE   (J.  E.):  Southern  Stellar  Objects  for  small  Telescopes, 

between   the   Equator  and    55°  south   declination;    with 

observations  made  in  the  Punjab.     Lodiana,  1877.     16mo. 
GOTHA  (observatory):  See  KRUEGER. 
[GOULD  (B.  A.)]:  Review  of  HERSCHEL'S  Outlines  of  Astronomy. 

Cambridge,  1849.     8vo.     P. 
:  History  of  the  Discovery  of  Neptune.    Washington,  1850. 

8vo.     P. 
:   Standard   Places  of   Fundamental    Stars.      2d  edition. 

Washington,  1866.     4to.     P. 
:  Reduction  of  D'AGELET'S  Observations  of  Fixed  Stars. 

Washington,  1866.     4to. 
:  The  Transatlantic  Longitude  (1866).    Washington,  1869. 

4to.     P. 
:  Uranometria  Argentina.    Text  and  maps.    Buenos  Aires, 

1879.     4to. 


Lick  Observatory  Library.  43* 

GOULD  (B.  A.):  Sobre  el  cometa  de  Mayo  de  1881.  n.  p.,  n.  d. 
8vo.  P. 

:  See  Cordoba. 

[ ] :  Addresses  at  the  complimentary  dinner  to  Dr.  GOULD. 

Lynn,  1885.  8vo.  P. 

GRABLOVITZ  (G.) :  Parere  Sugli  Avvisatori  Sismici.  Rome,  1888. 
folio.  P. 

:  Sopra  un  nuovo  principio  per  rendere  astatico  il  punto 

neutro  nei  sismografi.  Rome,  1888.  folio.  P. 

GRAF  (F.  E.  A.) :  Unsere  Erde  mit  ihrem  Monde.  Gotha,  1825. 
8vo. 

GRANT  (R.):  Catalogue  of  6415  Stars  (bound  in  2  vols.). 
Glasgow,  1883.  4to. 

GRASST  (G.):  See  Dictionary. 

GREEN  (F.  M.),  DAVIS  (C.  H.),and  NORRIS  (J.A.):  Telegraphic 
measurement  of  differences  of  longitude  (Greenwich — Lis- 
bon—S.  America).  Washington,  1880.  4to.  P. 

GREENHILL  (A.  G.):  Determination  of  the  greatest  height  con- 
sistent with  stability,  etc.  Cambridge,  n.  d.  8vo.  P. 

GREENWICH  (Royal  Observatory):  Annual  Catalogues  of  Stars, 
from  the  volumes  for  1851,  1855,  1857.  London.  4to. 

:  Astronomical  Results.  184- -7-8-9;  1850-1-2-3-5-6-7- 

8-9;  1860-1-2-3-4-5-6-7-8-9  (1860-69  bound  in  1  vol.); 
1870-1-2-3-4-5-6-7-8-9  (1870-75,  1  vol.;  1876-80, 1  vol.); 
1880-3-7-.  London.  4to.  P. 

:  Catalogues  of  Stars.     See  AIRY.     See  CHRISTIE. 

:  Introductions,  etc.    1877-8-9;  1880-3 — 7-.   London.   4to. 

:  Observations  for  the  years  1836-7-8-9;  184- -1-2-3-4-5- 

6-7-8-9;  1850-1-2-3-4-5-6-7-8-9;  1860-1-2-3-4-5-6-7- 
8-9;  1870-1-2-3-4-5-6-7-8-9;  1880-1-2-3-4-5-6-7.  Lon- 
don. 4to. 

:  Reduction  of  Lunar  Observations,  1750-1830  (2  vols.), 

1831-51  (1  vol.).  Reduction  of  Observations  of  Planets, 
1831-51;  also,  Appendix  II,  1864.  London.  4to. 

:  Reports  for  the  years  1836-80,  bound  in  2  vols.  London. 

4to. 

:  Report  for  1880,  1881,  1882,  1883,  1884,  1885,  1886,  1887, 

1888,  1889.  London.  4to.  P. 

:   R.  A.  of  Polaris,  from  the  vol.  for  1846.     London.     4to. 


44*  Catalogue  of  the 


GREENWICH  (Royal  Observatory):  Spectroscopic  and  Photo- 
graphic Results,  1878-84,  bound  in  1  vol.  Also,  1885-6-7- 
8-9.  London.  4to. 

:  Index  to  the  records  of  occasional  observations  and  cal- 
culations made  at  the  Royal  Observatory,  Greenwich,  and 
to  other  miscellaneous  papers  connected  with  that  Insti- 
tution, not  comprehended  in  the  ordinary  routine  of  the 
Observatory,  but  printed  in  the  Annual  volumes  of  the 
Greenwich  Observations  from  January,  1836,  to  December, 
1875,  with  a  list  of  other  publications  of  the  Royal  Observ- 
atory. [By  G.  B.  AIRY.]  See  Monthly  Notices  R.  A.  S., 
vol.  39,  p.  504.  (1879.)  8vo. 

GRIMES  (J.  S.):  Geonomy,  etc.     Chicago,  1881.     8vo.     P. 

GRUBB  (Sir  H.):  On  the  equatorial  telescope,  and  on  the  new 
observatory  of  the  Queen's  College,  Cork.  Dublin,  1879. 
8vo.  P. 

:  Description  of  the  Great  27-inch  Refracting  Telescope, 

etc.,  of  Vienna.  London,  1881.  folio. 

:  Telescopic  Objectives  and  Mirrors,  etc.  London,  1886. 

8vo.  P. 

:  On  the  latest  improvements  in  the  clock-driving  appa- 
ratus of  telescopes.  London,  1888.  8vo.  P. 

:  On  Great  Telescopes  of  the  Future,     n.p.,  n.  d.     4to.     P. 

[ ] :  Framed  photographs  of  Domes  and  telescopy  mount- 
ings made  by  him;  also  two  designs  for  the  LICK  Observa- 
tory installation  (date  about  1874). 

GUENTHER  (F.  W.):  De  perturbationibus  quas  Saturnus  in 
Palladem  exercet,  etc.  Breslau,  1860.  4to.  P. 

GUYOT  (A.):  The  Earth  and  Man.     Boston,  1855.     8vo. 

GYLDEN  (H.):  Relationer  emellan  stjernornas  glans,  etc. 
Stockholm,  1872.  8vo.  P. 

:  Ableitung  der  Declination  aus  den  am  Verticalkreise 

(1842-49)  angestellten  Beobachtungen.  St.  Petersburg, 
1873.  folio.  P. 

:  Die  Grundlehren  der  Astronomie.     Leipzig,  1877.     8vo. 

:  Undersokningar  af  Theorien  for  Himlakropparnas  rbrel- 

ser.  I.  Stockholm,  1881.  8vo.  P. 

:  Ueber  die  absoluten  Elemente  der  Planetenbahnen. 

Kiel,  1882.  4to.  P. 


Lick  Observatory  Library.  45* 

GLYDEN  (H.):  Om  ett  af  LAGRANGE  behandladt  fall  af  det  s.  k. 

trekrop-pars-problemet,  etc.     Stockholm,  1884.     8vo.     P. 
:  Theoretische   Untersuchungen  ueber  die   intermediaren 

Bahnen  der  Cometen,  etc.     St.  Petersburg,  1884.     folio. 
:  Untersuchungen  ueber  die  Convergenz  der  Reihen  welche 

zur  Darstellung  der  Cobrdinaten  der  Planeten  angewendet 

werden.     Stockholm,  1887.     4to.     P. 
:  Fortsatte  undersbkningar  rbrande  en  icke-linear  differ- 

entialeqvation    af    andra    ordningen.      Stockholm,    1888. 

8vo.     P. 

:  Om  Planetsystemets  Stabilitet.  Stockholm,  1888.  8vo.  P. 

:  On  the  relations   between  the  number,  brightness,  and 

relative  mean  distances  of  the  Stars  (translated  by  E.  S. 

HOLDEN  and  E.  BERGLAND).     n.  p.,  n.  d.    ,8vo.     P. 
HABENICHT  (H.):  Das  seismische  Problem.  Vienna,  n.d.  8vo.  P. 
HAGEN  ( J.) :  Die  Astronomic  in  den  letzten  Jahrzehnten.    Frei- 
burg (1888).     8vo.     P. 
and  HOLDEN  (E.S.):  A  Catalogue  of  1001  Southern  Stars 

for  1850,  from  observations  by  Signor  TACCHINT  in  1867-68- 

69,  etc.     Madison,  1882.     8vo.     P. 
HAINS  (P.  C.):  See  REYNAUD. 
HALL  (A.):  Observations  and  orbits  of  the  Satellites  of  Mars. 

Washington,  1878.     4to. 
:  Observations  of  the  Satellites  of  Mars.     London,  1880. 

8vo.     P. 
:  Note  on  the  Companion  of  Sirius.     New  Haven,  1880. 

8vo.     P. 
:  Address  before  the  A.  A.  A.  S.  (Section  A).    Boston,  1880. 

8vo.     P. 

:  Observations  of  Double  Stars.     Washington,  1881.     4to. 

:  The  Density  of  the  Earth,     n.  p.,  1882.     8vo.     P. 

— — :  Formulas   for   computing   the   position   of    a   Satellite. 

Washington,  1884.     8vo.     P. 

:  American  Scientific  Societies.  Washington,  1885.  8vo.  P. 

:  The  orbits  of  Oberon  and  Titania.     Washington,  1885. 

4to.     P. 
:  Orbit  of  the  Satellite  of  Neptune.      Washington,  1885. 

4to.     P. 
:  The  orbit  of  Japetus.     Washington,  1885.     4to.     P. 


46*  Catalogue  of  the 


HALL  (A.):  Variations  of  latitude.   New  Haven,  1885.   8vo.    P. 

:  The  six  inner  Satellites  of  Saturn.  Washington,  1886. 

4to.  P. 

:  Observations  for  Stellar  parallax.  Washington,  1886. 

4to.  'P. 

:  A  special  case  of  the  LAPLACE  coefficients.  Washington, 

1887.  8vo.  P. 

:  The  constant  of  aberration.     Cambridge,  1888.     4to.     P. 

and  HARKNESS  (W.):  Reports  on  Observations  of  ENCKE'S 

Comet  (1871).  Washington,  1872.  4to.  P. 

HALLEY  (E.):  EDMUNDI  HALLEII  Tabulae  Astronomicae.  Lon- 
don, 1749.  4to. 

HALMA  (N.  B.):  Hypotheses  et  Epoques  des  Planetes  de  C. 
PTOLEMEE,  etc.  Paris,  1820.  4to. 

HAMILTON  (W.  R,):  Elements  of  Quaternions.  London, 
1866.  8vo. 

HANSEN  (P.  A.):  Tables  de  la  Lune.     London,  1857.     4to. 

:  Untersuchungen  des  Weges  eines  Lichtstrahls  durch 

eine  beliebige  Anzahl  von  brechenden  Sphaerischen  ober- 
flaechen.  From  Vol.  X  Abhandlungen  der  K.  Sack.  GeselL, 
1871.  Translated  by  E.  S.  HOLDEN.  Ms.  [1878.]  4to. 

and  OLUFSEN:  Tables  du  soleil.     Copenhagen,  1853.     4to. 

HANSTEEN  (C.):  Untersuchungen  ueber  den  Magnetismus  der 
Erde.  Erster  Theil  (1  vol.  and  atlas).  Christiania,  1819. 
4to. 

:  Magnetischer  Atlas.     Christiania,  1819.     folio. 

and  DUE:  Resultate  magnetischer,  etc.,  beobachtungen 

(in)  Siberien,  1828-30.  Christiania,  1863.  4to. 

HARDWICH  (T.  F.):  A  manual  of  Photographic  Chemistry.  9th 
edition.  New  York,  1883.  12mo. 

HARKNESS  (Wm.):  Observations  on  Terrestrial  Magnetism,  etc., 
on  the  U.  S.  iron-clad  Monadnock.  Washington,  Smith- 
sonian Institution,  1873.  4to.  P. 

:  Theory  of  the  horizontal  photoheliograph,  and  supple- 
mentary note.  Boston,  1877.  8vo.  P. 

:  On  the  physical  configuration  of  Mars.  London,  1879. 

8vo.  P. 


Lick  Observatory  Library.  47* 

HARKNESS  (Wm.):  On  the  color  correction  of  achromatic  tele- 
scopes. Salem,  1879.  8vo.  P. 

:  Same]  a  reply  to  Professor  HASTINGS.  New  Haven, 

1880.  Svo.  P. 

:  Note  on  the  observations  of  Comet  '&,  1881,  made  at  the 

U.  S.  N.  0.  New  Haven,  1881.  Svo.  P. 

:  On  the  flexure  of  meridian  instruments.  Washington, 

1886.  4to.  P. 

HARLEM  (Musee  Teyler):  Archives.  Series  II;  Vols.  1,  2,  3 
(1880-89),  bound  in  1  vol.  Harlem.  Svo. 

:  Catalogue  de  la  Bibliotheque.     Harlem,  1885.     Svo. 

HARLEM  (Societe  Hollandaise  des  Sciences):  Archives.  Vol.  23 
(1888),  24. 

HARTING  (J.):  Untersuchungen  ueber  den  Lichtwechsel  des 
Sternes  Beta  Persei.  Munich,  1889.  4to.  P. 

HARZER  (P.):  Ueber  ein  dreiflaechiges  *  *  *  Objectiv. 
Kiel,  1886.  4to.  P. 

:  Untersuchungen  ueber  einen  Speciallen  Fall  des  Prob- 
lems der  Drei  Koerper.  St.  Petersburg,  1886.  folio.  P. 

HASSELBERG  (B.):  Ueber  das  durch  electrische  Erregung 
erzeugte  Leuchten  der  Gase  bei  niedriger  Temperatur.  St. 
Petersburg,  1879.  folio.  P. 

:  Ueber  die  Spectra  der  Cometen.  St.  Petersburg,  1880. 

folio.  P. 

:  Zur  Spectroskopie  des  Wasserstoffs.  St.  Petersburg,  1880. 

Svo.  P. 

:  Untersuchungen  ueber  das  Zweite  Spectrum  des  Wasser- 
stoffs. Parts  I,  II.  St.  Petersburg,  1882-3.  folio.  P. 

:  Zur  Spectroskopie  des  Stickstoffs.  I.  St.  Petersburg, 

1885.  folio.  P. 

:  Sur  un  methode  propre  a  determiner  les  longueurs  d'onde 

des  raies  ultra- violettes.  Rome,  1886.  folio.  P. 

HASTINGS  (C.  S.):  A  General  Method  for  determining  the  sec- 
ondary chromatic  aberration,  etc.  New  Haven,  1889. 
Svo.  V. 

:  See  HOLDEN. 

HASWELL  (C.  H.):  Mechanics'  and  Engineers'  Pocket  Book. 
54th  edition.  New  York,  1890.  12mo. 


48*  Catalogue  of  the 


HAYDEN  (E.):  The  Great  Storm  *  *  *  of  March  11-14, 
1888  [in  the  N.  E.  States].  Washington,  1888.  4to.  P. 

HAYES  (I.  I.):  Physical  Observations  in  the  Arctic  Seas.  Re- 
duced by  C.  A.  SCHOTT.  Washington,  Smithsonian  Insti- 
tution. 4to.  P. 

HAYN(F.):  Bahn-bestimmung  des  Cometen  1862,111.  Leip- 
zig, 1889.  4to.  P. 

HEAP  (D.  P.):  Report  on  the  International  Exhibition  of 
Electricity.  Washington,  1884.  8vo. 

HEINFOGEL  (C.):  See  DURER. 

HEIS  (E.):  Atlas  coelestis  novus.  1  vol.  text  and  atlas.  Co- 
logne, 1872.  16mo. 

HELMHOLTZ  (H.):  Optique  physiologique.  Translated  by  E. 
JAVAL  and  N.  T.  KLEIN.  Paris,  1867.  8vo. 

HELSINGFORS  (observatory):  See  KRUEGER. 

HENNERT  (T.  F.):  See  Berlin. 

HENNESSY  (H.):  Note  on  the  annual  precession,  calculated  on 
the  hypothesis  of  the  Earth's  solidity.  London,  1886. 
8vo.  P. 

HENRIVAUX  (J.):  Le  Verre  et  le  Cristal.     Paris,  1883:    8vo.   P. 

[HENRY  (J.)]:  See  TAYLOR. 

HERENY  (observatory):  Publikationen.  Heft  I  (1883).  Hereny, 
1884.  4to.  P. 

HERSCHEL  (A.)  (pseudonym) :  Der  Zusammenstoss  unserer  Erde 
mit  dem  Kometen  am  13ten  Juni,  1857;  Eine  Vorlesung 
von  Dr.  A.  HERSCHEL.  Motto.  Sie  geht  doch  unter, 
Altona  and  Hamburg,  1857.  Svo.  P. 

HERSCHEL  (A.  S.)  and  others:  Report  of  observations  of  Lumi- 
nous Meteors,  1878-9  (B.  A.  A.  S.).  London,  1879.  Svo.  P. 

:  Observations  of  earth  tremors,  etc.;  also,  on  an  improved 

form  of  Seismoscope.  Newcastle,  1888.  Svo.  P. 

HERSCHEL  (J.):  Results  of  Astronomical  observations  made 
during  1834-5-6-7-8  at  the  Cape  of  Good  Hope.  London, 
1847.  4to. 

:  A  Catalogue  of  10300  Double  Stars,  edited  by  R.  MAIN 

and  C.  PRITCHARD.  London,  1874.  4to. 

and  SOUTH  (J.):  Observations  of  380  Double  Stars.  Lon- 
don, 1825.  4to. 


Lick  Observatory  Library.  49* 

[HERSCHEL    (J.    F.    W.)]:    Large   lithographed   copy    of  Mrs. 

CAMERON'S  photographed  portrait. 
HERSCHEL  (W.):  1.  On  Satellites  of  Saturn.      P.  T.,  1790.     2. 

On  Spherical  Motion  (by  C.WILDBORE).    P.  T.,  1790.    3.  On 

Satellites  of  Uranus.     P.  T.,  1815.     4.  On  changes  in  the 

relative  position  of  Double  Stars.     P.  T.,  1804.     Bound  in 

1  vol.     London.     4to. 
— — :  Ueber  den  Bau  des  Himmels  (atlas  only),     n.  p.,  n.  d. 

oblong  folio. 
:  Ms.,  copies  of  four  musical  compositions  by  Sir  WILLIAM 

HERSCHEL.     1.  Glee.     2.  "Thou,  chiefly  thou."     3.  Echo 

Catch.     4.  Favorite  Catch.     (Presented  byE.  S.  HOLDEN.) 

Ms. 

[ — ; — ] :  Life  of.     See  HOLDEN. 
HERZ    (N.):    Siebenstellige  logarithmen  der  trigonometrischen 

functionen  fur  jed'e  zeitsecunde.     Leipzig,  1885.     8vo. 
and  STROBL  (J.):    Reduction  des  AUWERS'  schen  Funda- 

mentalcataloges  auf  die  LE  VERRIER'  schen  Praecessions- 

coefiicienten.     Vienna,  1883.     4to. 

HEVELIUS:  [Extracts  from].     Machina   Celestis.     See  PRINCE. 
HILPICKER  (J.):  Ausgleichung  des  Langennetzes  der  Europae- 

ischen  Gradmessung.     Kiel,  1885.     4to.     P. 
:  Sur  la  marche  de   la   pendule   astronomique  WINNERL. 

Neuchatel,  1886.     8vo.     P. 
:  L'influence  de  la  pression  de  1'air  sur  la  marche   des 

chronometres.     Neuchatel,  1889.     8vo.     P. 
:  Sur  une   Equation   Personnelle   dans    les   observations 

de  passage.     Neuchatel,  1889.     8vo.     P. 
HILGER  (A.):  A  new  form  of  governor  for  the  driving  clocks  of 

equator  ials.     London,  1886.     8vo.     P. 
HILL  (C.  B.):  Astronomical  photography,  a  lecture,  etc.     San 

Jose,  1889.     8vo.     P. 

HILL  (G.  W.):  Tables  of  Venus.     Washington,  1873.     4to. 
:  On  the  part  of  the  motion  of  the  lunar  perigee,  which  is 

a  function  of  the  mean  motions  of  the  Sun   and   Moon. 

Cambridge,  1877.     4to.     P. 
:  On  GAUSS'S  method  of  computing  secular  perturbations. 

Washington,  1881.     4to.     P. 


50*  Catalogue  of  the 


HILL  (G.  W.):  Lunar  inequalities  due  to  the  ellipticity  of  the 

earth.     Washington,  1884.     4to.     P. 
:  On  certain  lunar  inequalities  due  to  the  action  of  Jupiter. 

Washington,  1885.     4to.     P. 
:  A  new  theory  of  Jupiter  and  Saturn.    (Astron.  Papers  of 

the  Amer.  Ephem.,  Vol.  4.)     (Washington),  (1890).    4to. 
HIMMEL  UND  ERDE:  Vol.  I  (1889);  II  (current).    Berlin.    8vo. 
HIND  (J.  R.):  The  Solar  System.     New  York,  1852.     8vo. 
HIRN  (G.   A.):  La  conservation   de   1'energie  Solaire.     Paris, 

1883.     8vo.     P. 
:  Expose  d'un  moyen  de  determiner  la  temperature    *     * 

du  Soleil.     Paris,  1885.     8vo.     P. 
:  Causes  de  la  detonation  des  Bolides,  etc.     Paris,  1886. 

8vo.     P. 

:  La  cinetique  moderne  et  le  dynamisme  de  Pavenir.  Brus- 
sels, 1886.     8vo.     P. 
HIRSCH  (A.):  See  PLANTAMOUR. 

HIRSCH  (Meier):  Integraltafeln.     Berlin,  1810.     4to. 
HOEFER  (F.):  Histoire  de  P Astronomic.     Paris,  1873.     8vo. 
HOEK    (M.):     Recherches     astronomiques    de    1'observatoire 

d'Utrecht.     Parts  1-2,  bound  in  1  vol.     La  Haye,  1861-64. 

4to. 
HOLETSCHEK  ( J.) :  Ueber  die  Bahn  eines  Kometen,  der  wahrend 

seiner  gunstigen  Helligkeit  nicht  aus  den  Sonnenstrahlen 

heraustreten  Kann.     Vienna,  1883.     8vo.     P. 
:  Ueber  die  Richtungen  der  grossen  Axen  der  Kometen- 

bahnen.     Vienna,  1886.     8vo.     P. 
:    Ueber  die  Frage  nach  der  Existenz  von  Kometensytemen. 

Vienna,  1887.     8vo.     P. 
HOLDEN  (E.  S.):  On  supposed  changes  in  the  Nebula  M.  17 

(G.  C.  4403).     New  Haven,  1876.     8vo.     P. 
:  On  the  number  of  words  used  in  speaking  and  writing 

(from    Bulletin   Phil.    Soc.,    Washington).      Philadelphia, 

1876.  8vo.     P. 

:  Index-Catalogue   of    Books    and    Memoirs    relating   to 

Nebulae  and  Clusters,  etc.     Washington,  1877.     8vo. 
:  On  the  proper  motion  of  the  trifid  nebula.     New  Haven, 

1877.  8vo.     P. 


Lick  Observatory  Library.  51* 

HOLDEN  (E.  S.):  Note  on  the  reticulated  forms  of  the  Sun's 

surface.     New  Haven,  1878.     8vo.     P. 
:  Index  Catalogue  of  Books  and  Memoirs  on  the  Transits 

of  Mercury.     Cambridge,  1878.     8vo.     P. 
:  Catalogue  of  the  library  of  the  U.  S.  Naval  Observatory, 

Part  I.     Washington,  1879.     4to.     P. 
:  A  Subject-Index  to  the  Publications  of  the  U.  S.  Naval 

Observatory,  1845-75.     Washington,  1879.     4to.     P. 
:  Annual  Record  of  Astronomy,  1878.     New  York,  1879. 

8vo.     P. 
:    Reports   of  Observatories,  1879  (edited   by  E.  S.  H.). 

Washington,  1880.     8vo.     P. 
:  Note  on  a  relation  between  the  Colors  and  Magnitudes 

of  the  Components  of  Binary  Stars.     New  Haven,  1880. 

8vo.     P. 

:  Studies  in  Central  American  Picture  Writing.     Wash- 
ington, 1881.     8vo. 
:  Report  of  the  Eclipse   Expedition   to  Caroline  Island, 

May,  1883.     Washington,  1883.     4to. 
:    Observations   of    Comet   6,    1881.     New   Haven,    1881. 

8vo.     P. 
:  Sir  W.  HERSCHEL;    His  Life  and  Works.     New  York, 

1881.     Svo. 
.  *     *     *    Telescopes  used  as  night  glasses.     New  Haven, 

1881.  Svo.     P. 

:  The  Multiple  Star  STRUVE  748.     Washington,  1881.     4to. 

:  Investigation  of  the  Objective   and  Micrometer  of  .the 

26-inch  Equatorial.     Washington,  1881.     4to. 
:  Monograph  of  the  Central  Parts  of  the  Nebula  of  Orion. 

Washington,  1882.     4to. 
:  Figure  of  the  Nucleus   of  the   Bright   Comet   of  1882. 

New  Haven,  1882.     Svo.     P. 
:  An  account  of  the  Progress  of  Astronomy  in  the  year 

1882.  Washington,  1883.     Svo.     P. 

:    Observations    of    the   Transit    of    Venus,    1882.      New 

Haven,  1883.     Svo.     P. 
:  The  Three  HERSCHEL s  (from  the  Century).     New  York, 

1885.     Svo.     P. 
:  Sketch   of    Professor   S.    P.    LANGLEY    (from   Pop.    Sci. 

Monthly).     New  York,  1885.     Svo.     P. 


5'2*  Catalogue  of  the 


HOLDEN  (E.  S.):  Photography  the  Servant  of  Astronomy. 
San  Francisco,  1886.  8vo.  P. 

:  List  of  recorded  earthquakes  in  California,  Lower  Cali- 
fornia, Oregon,  and  Washington  Territory  (1769-1887). 
Sacramento,  1887.  8vo. 

:  (XIX  charts,  showing  the  density  of  the  Stars  in  the  S.  D., 

from  Professor  SEELIGER'S  counts.  Ms.)}  bound  in  1  vol. 

1887.  folio. 

:  The  Ring  Nebula  in  Lyra.     London,  1888.     8vo.     P. 

:  Earthquakes  in  California,  1769  to  1888,  arranged  alpha- 
betically by  towns.  Manuscript,  n.  p.,  1888.  folio.  P. 

:  The  total  Solar  Eclipse  of  1889,  January  1.  Probable 

meteorological  conditions  at  that  time.  London,  1888. 
Svo.  P. 

:  Handbook  of   the  Lick  Observatory.      San    Francisco, 

1888.  16mo. 

:  Note  on  earthquake  intensity  in  San  Francisco  (1808-88). 

New  Haven,  1888.     8vo.     P. 
:  Earthquakes  in   California  (1888).     New  Haven,  1889. 

8vo.     P. 

:  On  the  Solar  Eclipse  of  January  1, 1889  (frornjhe  Observ- 
atory, March,  1889).     London,  1889.     8vo.     P. 
:  On  the    Photographs  of  the  Corona,  January  1,  1889. 

London,  1889.     8vo.     P. 
:  On  some  of  the  features  of  the  arrangement  of  Stars  in 

Space.     London,  1890.     Svo.     P. 
:  The  photographic  apparatus  of  the  great  Equatorial  of 

the  Lick  Observatory.     London,  1890.     8vo.     P. 
:  Account  of  the  Progress  of  Astronomy  for  1879-80, 1881, 

1882,  18§3,  1884  (from  Smithsonian  Reports),  (bound  in  1 

vol.).     Washington.     Svo. 
:  Auxiliary  table  for  computing  refractions.    Washington, 

n.  d.     4to.     P. 
:  Earthquakes  in  California  and  elsewhere  (from  Overland 

Monthly).     San  Francisco.     Svo.     P. 

:  Stellar  Photography.     San  Francisco,  n.  d.     Svo.     P. 

:  List  of  (77)  Red  Stars,  etc.     Dublin,  n.  d.     4to.     P. 

:  Card  catalogue  of  4592  YARNALL  Stars  reduced  to  1850.0; 

also,  Card  catalogue  of  39000  Washington  Zone  Stars.    Ms. 


Lick  Observatory  Library.  53* 

HOLDEN  (E.  S.):  Plan.of  a  Dome  of  75  feet  diameter.     (1885.) 

(framed  drawing.) 
:  See  GYLDEN.     See  HAGEN.     See  HANSEN.     See  LANG  LEY. 

See  Madison  (Washburn  Observatory).    See  NEWCOMB.    See 

Washington  (U.  S.  Naval  Observatory).     See  WINLOCK. 
and  HASTINGS  (C.  S.):  A  Synopsis  of  the  scientific  writings 

of  Sir  WILLIAM  HERSCHEL.     Washington,  1881.     8vo. 
and  SCHAEBERLE  (J.  M.):  Observations  of  Nebulae  at  the 

Lick  Observatory.     London,  1888.     8vo.     P. 
HOMANN    (H.):   Beitraege   zur   Untersuchungen   der   Sternbe- 

wegungen    und    der   Lichtbewegungen    durch     Spektral- 

messungen.     Berlin,  1885.     4to.     P. 
HONGKONG    (observatory):    Observations,  1884-5-6-7-8,  bound 

in  1  vol.     Hongkong,     folio. 

HOPKINSON  (J.):  The  residual  charge  of  a  Leyden  jar.     Lon- 
don, 1876.     4to.     P. 
HORNSTEIN  (C.):   Ermittlung  der  Refractions-Constanten  von 

Palermo    aus    PIAZZI'S    Beobachtungen.      Vienna,    1851. 

4to.     P. 
:    Planeten     und     Cometen-Beobachtungen      (1860-62). 

Vienna.     8vo.     P. 

:  See  JELINEK. 

HOUZEAU  ( J.  C.) :  Vade  Mecum  de  PAstronorne.     Brussels,  1882. 

Svo. 
and  LANCASTER  (A.):  Bibliographic  generale  de  1'astrono- 

mie.     Vol.  I,  Part  I  (1887).  Vol.  II  (1882).  Brussels,  1882. 

Svo. 
:  Note  sur  un  methode  pour  determiner  la  constante  de 

Faberration.     Brussels,  1887.     Svo.     P. 
HOWE  (H.  A.) :  Total  Solar  Eclipse  of  January  1, 1889.    Denver, 

1889.     Svo.     P. 

:  *     *     *     KEPLER'S  problem.    Cincinnati,  n.  d.    Svo.    P. 

HUGGINS  (W.):  Note  on  the  Heat  of  the  Stars.     London,  1869. 

Svo.     P. 
— — :  Note  on  a  method  of  viewing   the   Solar   prominences 

without  an  eclipse.     (1  leaf.)     London,  1869.     Svo.     P. 
:  Note  on    the   Spectra   of  Erbia.,   etc.      London,   1870. 

Svo.     P. 


54*  Catalogue  of  the 


HUGGINS  (W.):  The  photographic  Spectra  of  the  Stars.  Lon- 
don, 1880.  8vo.  P. 

:  On   the   photographic   Spectra   of  the   Stars.     London, 

1880.     4to.     P. 

:  On  the  Spectrum  of  the  Flame  of  Hydrogen.     London, 

1880.     8vo.     P. 

:  Preliminary  note  on  the  photographic  Spectrum  of  Comet 

6,1881.     London,  1881.     Svo.     P. 

:  On  the  function  of  the  Sound  post     *     *     *     (in)  the 

Violin.     London,  1883.     Svo.     P. 

:  On  the  Corona  of  the  Sun.     London,  1885.     Svo.     P. 

:  On  the  limit  of  Solar  and  Stellar  Light  in  the  ultra- 
violet part  of  the  Spectrum.  London,  18S9.  Svo.  P. 

:  (Photograph  of  the  Solar  Corona  of  April  24,  1888,  taken 

in  full  daylight.)     (Photograph  of  a.  pseudo-corona  due  to 
air  glare.)     2  photographs. 

and  MILLER  (W.  A.):  On  the  Spectrum  of  a  new  Star  in 

Corona  Borealis.     London,  1856.     Svo.     P. 

and  Mrs.  HUGGINS:  Note  on  the  photographic  Spectra  of 

Uranus  and  Saturn.     London,  1S89.     Svo.     P. 

HUMBOLDT  (A.  von):  Cosmos:  A  sketch  of  a  physical  descrip- 
tion of  the  Universe.  Translated  from  the  German  by 
E.  C.  OTTE.  5  vols.  London,  1849-58.  Svo. 

[HUMBOLDT  (A.)]:  A  Biographical  Monument,  by  Prof.  KLENKE. 
London,  1852.  Svo. 

et  BONPLAND  ( ):  Voyage  de  HUMBOLDT  et  BONPLAND; 

Astronomic.     2  vols.     Paris,  1810.     4to. 

HUTCHINS  (C.  C.):  An  account  of  *  *  *  some  measures  of 
lunar  radiation.  Boston,  1889.  Svo.  P. 

HUTTON  (C.):  Philosophical  and  Mathematical  Dictionary. 
Vols.  I,  II.  London,  1815.  4to. 

:  See  London  (Royal  Society). 

HYDE  (E.  W.):  The  Directional  Calculus.     Boston,  1890.    Svo. 

ICONOGRAPHIC  ENCYCLOPAEDIA:  4  vols.  text,  2  vols.  plates.  New 
York,  1852.  4to. 

IDELER  (L.):  Lehrbuch  der  Chronologie.     Berlin,  1831.     Svo. 
[INSTRUMENTS]:  Catalogue  of  Instruments.  English  and  Ameri- 
can, 1  vol.     Svo.     German,  1  vol.     Svo. 


Lick  Observatory  Library.  55* 

(The)  INTELLECTUAL  OBSERVER:  Vols.  1,  2,  3,  4,  5,  6,  7,  8,  9,  10, 
11,12.  [Temporarily  lent  to  the  L.  0.  by  S.  W.  BURNHAM.] 
London,  1862-68.  Svo. 

JACKSON  (L.  D'A.) :  Simplified  Weights  and  Measures.  London, 
1876.  Svo.  P. 

JACQUES  ( W.  W.):  Distribution  of  Heat 'in  the  Spectra  of  Vari- 
ous Sources  of  Radiation.  Cambridge,  1879.  Svo.  P. 

JAMES  (G.  W.):  The  Lick  Observatory.  A  Guide  Book.  San 
Francisco,  1887.  Svo.  P. 

JAMES  and  GRASSI:  See  Dictionary. 

JAMIN  (J.):  Cours  de  Physique.     Vol.  III.     Paris,  1866.     Svo. 

JANSSEN  (J.):  Note  sur  les  passages  des  Corps  *  *  *  sur 
le  Soleil.  Paris,  1876.  4to.  P. 

:  Sur  les  photographies  des  nebuleuses.    Paris,  1881.  4to.  P. 

:  Note  sur  les  raies  telluriques  et  le  Spectre  de  la  vapeur 

d'eau.  Paris,  1882.  4to.  P. 

:  Note  sur  1'observation  du  passage  de  la  planete  Venus 

sur  le  Soleil.  Paris,  1883.  4to.  P. 

JELINEK  (C.)  and  HORNSTEIN  (C.):  Cometen-Beobachtungen 
(1835-6  and  1843-6).  Vienna,  n.  d.  4to. 

JENKIN  (F.):  Electricity  and  Magnetism.  8th  edition.  Lon- 
don, 1885.  16mo. 

JENNEY  (W.  P.):  See  NEWTON. 

JIMENEZ  (F.)  and  FERNANDEZ  (L.):  Determinacion  de  la  longi- 
tude del  pendulo  de  segundos  en  Mexico.  Mexico,  1880. 
Svo.  P. 

JOHNSON  (W.  W.):    An   elementary   treatise   on   the  Integral 

Calculus.     New  York,  1888.     Svo. 

:  See  RICE. 

JOHNSON    (M.  J.):   First    Radclifte   Catalogue  of  6317   Stars. 

Oxford,  1860.     Svo. 
JOSEPHUS   (Pater)   (pseudonym}:   Der  Komet  vom  1857,  oder 

die  alte  Propheziehung  vom  Untergang  der  Welt,  welcher 

am   13   Juni,  1857,  ganz  gewiss  erfolgen   wird,  etc.,  etc. 

Berlin.     16mo.     P. 
JOURNAL  DU  CIEL:  Bulletin   de   la   Societe   d'Astronomie    (de 

Paris).     Directeur,  J.   VINOT.     Beginning  with  No.   1046 

(March  16,  1891).     Paris,  1891-     Svo. 
12 


56*  Catalogue  of  the 


JULIEN  (C.  E.):  See  SCHMITZ. 

KAISER  (F.):  Verhandeling  over  de  Komeet  van  HALLEY,  etc. 
Amsterdam,  1835.  8vo. 

:  De  Kometen  van  de  Jaren,  1556-1264  en  975  en  Hare 

Vermeende  identiteit.     'S  Gravenhage,  1857.     4to. 

KALOCSA  (observatory):  [ Publications]  I,  II  (1886);  III  (1887); 
IV  (1888).  8vo.  P. 

KAM  (N.  M.):  Catalog  von  Sternen  *  *  *  aus  Band  1  bis 
66  der  Astronomische  Nachrichten  (1855.0).  Amsterdam, 
1885.  4to. 

KANE  (E.  K.):  Magnetic  Observations  in  the  Arctic  Seas.  Re- 
duced by  C.  A.  SCHOTT.  Washington,  Smithsonian  Insti- 
tution, 1858.  4to.  P. 

:  Meteorological  Observations  in  the  Arctic  Seas  in  1853- 

54-55.     Reduced  by  C.  A.  SCHOTT.      Washington,  Smith- 
sonian Institution,  1859.     4to.     P. 

:  Astronomical  Observations  in  the  Arctic  Seas.     Reduced 

by  C.  A.  SCHOTT.     Washington,  Smithsonian  Institution, 
1860.     4to.     P. 

KANT  (I.):  Allgemeine  Naturgeschichte  und  Theorie  des  Him- 
mels.  Zeiss,  1798.  8vo. 

KAPTEYN  (J.  C.):  Bericht  ueber  die  zur  Herstellung  einer 
Durchmusterung  des  siidlichen  Himmels  ausgefiihrten 
Arbeiten.  Leipzig,  n.  d.  8vo.  P. 

KARLSRUHE  (observatory) :  Veroejfentlichungen,  Vol.  III.  Karls- 
ruhe, 1889.  4to. 

:  See  Mannheim. 

KASAN  (observatory):  Observations  des  etoiles  de  la  Zone 
entre  +75°  et  +80°.  Vols.  I,  II.  Kasan,  1885  and  1887. 
8vo. 

KEELER  (J.  E.):  L'aspect  de  Saturne  dans  1'equatorial  de  1'ob- 
servatoire  Lick  (from  del  et  Terre).  Brussels,  1889. 
8vo.  P. 

:  On  the  motions  of  the  planetary  nebulae  in  the  line  of 

sight.     San  Francisco,  1890.     8vo.     P. 

:  See  SCHIAPARELLT. 

KELLAND  (P.)  and  TAIT  (P.  G.):  Introduction  to  Quaternions. 
2d  edition.  London,  1882.  8vo. 


Lick  Observatory  Library.  57* 

KIEL    (observatory):  .  Publicationen    (indexed     separately   by 

authors).     Kiel.     4to. 

:  See  KRUEGER,  KREUTZ,  LAMP,  KLOOCK. 

KING  (C.):  See  Washington  (U.  S.  Geological  Survey). 
KIRCHHOFF   (G.):    Vorlesungen  ueber  Mathematische  Physik 

(Mechanik).     Leipzig,  1883.     8vo. 
KIRKWOOD  (D.):  On  Meteoric  Fireballs  seen  in  the  U.  S.  during 

1879.  Philadelphia,  1879.     8vo.     P. 

:  BIELA'S  Comet  and  the  large  meteors  of  Nov.  27-30. 

Philadelphia,  1887.  8vo.  P. 

:  The  Asteroids  (with  JHS.  additions  by  the  author).  Phila- 
delphia, 1888.  8vo. 

:  On  the  inclinations  of  the  Asteroids.  Philadelphia,  1889. 

8vo.  P. 

KIS-KARTAL  (observatory).     See  KOVESLIGETHY. 

KITCHENER  (F.  E.):  Geometrical  Note  Book.  London,  1882. 
4to.  P. 

KLEIN  (H.  J.):  Tafeln  zur  Bestimmung  der  Lichtgrenze  auf  der 
Mondscheibe  (from  Sirius,  Band  XIII,  1880).  Leipzig, 

1880.  8vo.     P. 

:  Star  Atlas,  English  edition  by  E.  McCLURE.     London, 

1888.     4to. 
KLENKE  (Professor):  See  HUMBOLDT. 

KLINKERFUES    (W.):    Theoretische    Astronomie.      Brunswick, 

1871-2.     8vo. 
-:  Ueber  die  Kometen-Erscheinungen  von  371  v.  Chr.,  1668, 

1843  I  und  1880  I.     Gottingen,  1880.     8vo.     P. 
KLOOCK  (H.):  Tafel  fuer  das  3  Glied  der  Praecession.      Kiel, 

1890.     4to. 

KNOWLEDGE:  Vols.  XII  (1889);  XIII  (current).    London.     4to. 
KOENIGSBERG  (observatory ) :  Astronomische  Beobachtungen  auf 

der  K.  Universitats-Sternwarte  in  Konigsberg.    Vols.  (1-3), 

1813-17;  vols.  (4-6),  1817-21;  vols.  (7-9),  1821-24;  vols. 

(10-12),  1824-27;   vols.  (13-15),  1827-30;   vols.  (16-18), 

1830-33;   vols.  (19-21),  1833-36;  vols.  (22-24),  1836-39; 

vols.  (25-26),  1839-42;  vol.  (27),  1842-44;  vols.  (28-30), 

1844-48;  vols.  (31-32),  1848-55;  vols.  (33-34),  1855-58; 

vols.  (35-36),  1865-70;  vol.  37  (i,  ii),  1882-86.     Bound  in 

15  vols.     Koenigsberg.     folio. 


58*  Catalogue  of  the 


KOBOLD  (H.):  KLINKERFUES' sche  Neue  Constante  (lithograph). 

2  vols.     O-Gyalla,  1880  and  1881.     4to.     P. 

:  Same  for  1884.     Gottingen,  n.  d.     8vo.     P. 

KOERBER  (F.):    Ueber   den    Cometen   1866  I.     Breslau,   1887. 

8vo.     P. 
KOVESLIGETHY  (R.  von):  Grundziige  einer  theoretischen  Spec- 

tralanalyse.     Halle,  1890.     8vo. 
KONKOLY   (N.  von):  Das  Object! vprisma,   etc.     Vienna,  1888. 

8vo.     P. 

:  See  O-Gyalla. 

KNIPPING  (E.):  Report  of  an  expedition  to  Mount  Fuji.    Tokio, 

1887.     8vo.     P. 
KNOBEL  (E.  B.):  Note  on  Jupiter,  1873.     Notes  on  Mars,  1873. 

London,  1873.     8vo.     P. 

:  Observations  of  Jupiter,  1874.     London,  1874.     8vo.     P. 

:  Reference    Catalogue  of  Astronomical   Papers   and  Re- 
searches.    London,  1876.     8vo.     P. 
:  Notes  on  Mr.  BURNHAM'S  paper  entitled  "  Examination 

of  the  Double  Star  Measures  of  the  Bedford  Catalogue." 

London,  1880.     8vo.     P. 
:  Notes  on  Sketches  of  Comet   6,  1881.      London,  1881. 

8vo.     P. 

:  On  a  new  astrometer.     London,  n.  d.     8vo.     P. 

KOWALSKI  (M.):    See  Kasan. 

KRAKOW   (observatory):   Stan  Wody  na  Rzekach  Galicyjskich 

oraz  Opad  Atmosferyczny,  etc.,  1887-88.    Krakow.  8vo.  P. 
KREMSER    (V.):    Die  Bahn   des   zweiten   Cometen   von    1879; 

Breslau,  1883.     8vo.     P. 
KREUTZ  (H.):  Untersuchungen  ueber  die  Bahn  des  Kometen 

1861  II.     Bonn,  1880.     4to.     P. 

:  Ueber  die  Entwickelung  der  Stellarphotographie.     Tu- 
bingen, 1887.     8vo.     P. 
:  Untersuchungen  ueber  das  Cometensystem  1843  I,  1880 

I,  und  1882  II.     I  Thiel.     Kiel,  1888.     4to.     P. 
KRUEGER   (A.):    Ueber  die  parallaxe  des  Sternes  LI.  21258. 

Helsingfors,  1863.     4to.     P. 
:  Untersuchungen   ueber  die  Bahn  des  planeten    Themis. 

Fortsetzung.     Helsingfors,  1873.     4to.     P. 


Lick  Observatory  Library.  59* 

KRUEGER    (A.):    Zonenbeobachtungen    der    Sterne    zwischen 

+55°  und    +65°,  etc.     [Helsingfors-Gotha   Zone.]     Vol. 

I  (1883);  II  (1885).     Helsingfors.     4to. 
:  Anhang  zu  den   Zonnenbeobachtungen   -f~55°  to  -|-650, 

etc.     Kiel,  1890.     4to.     P. 
KUESTNER  (F.):  Resultate  aus  Beobachtungen  von  670  Sternen 

angestellt  (1885-86)  am  grossen  Berliner  Meridian  Kreise. 

Berlin,  1887.     4to.     P. 
:  Neue  Methode   zur   Bestimmung   der   Aberrations-Con- 

stante,  etc.     Berlin,  1888.     4to.     P. 
LACAILLE  (N.  L.):    Catalogue  of  9766  Stars.     Reduced  by  F. 

BAILY  and  T.  HENDERSON.     London,  1847.     8vo. 
LACHMANN  (G.):  Ueber  die  Bahn  des  Planeten  (79).     Breslau, 

1884.     8vo.     P. 
LAGRANGE  (J.  L.):  Oeuvres  de  LAGRANGE  publiees  par  les  soins 

de  J.  A.  SERRET,  etc.     Vol.  I  (1867);  II  (1868).     Paris. 

4to.     [Loaned  to  the  L.  0.  by  GEORGE  F.  BECKER,  Ph.D.] 
LAING  (S.):  LOCKYER'S  Meteorite  Theory  (from  Contemporary 

Review).     London,  1888.     8vo.     P. 
LALANDE   (J.  F.):  Astronomie.     3d  edition.     Vols.  I,  II,  III. 

Paris,  1792.     4to. 

:  Histoire  Celeste  Franchise.     Paris,  1801.     4to. 

:  Bibliographic  astronomique  avec  1'histoire  de  F Astrono- 
mie, 1781-1802.     Paris,  1803.     4to. 
:  Catalogue  of   Stars  in  the  Histoire  Celeste  Franchise. 

Reduced  by  F.  BAILY.     London,  1847.     8vo. 
LALANDE  (J.  de):  See  FEDORENKO. 
LAMEY  (M.):  Systeme  Geologique  Eruptif  de  la  planete  Mars. 

Autun,  1884.     8vo.     P. 
LAMP  (E.):    Das  Aequinoctium  fur  1860.0,  etc.     Kiel,  1882. 

4to.     P. 
LAMP  (J.):  Neue  Berechnung  der  Parallaxe  von  61  Cygni  aus 

den  Beobachtungen  von  SCHWEIZER  (1863-66).    Kiel,  1883. 

8vo.     P. 
LAMONT    (J.):     Magnetische    Ortsbestimmungen,    etc.      I-II. 

Munich,  1854-56.     8vo. 

:  Astronomischer  Kalender,  1850-51-52-53.    1  vol.    Mu- 
nich.    8vo. 


60*  Catalogue  of  the 


LAMONT   (J.):    Untersuchungen   ueber     *     *     *     Erdmagnet- 

ismus,  etc.     Munich,  1859.     4to. 

:  Handbuch  des  Erdmagnetismus.     Berlin,  1849.     8vo. 

:  Untersuchungen   ueber   die    Richtung   und   Starke   des 

Erdmagnetismus.  etc.     Munich,  1858.     4to. 
:  Verzeichniss  von  9412  Sternen,  +3°  bis  — 3°.     Munich, 

1866.     8vo. 
:  Verzeichniss  von  4793  telescopischen  Sternen,  — 3°  bis 

—9°.     Munich,  1869.     8vo. 
-:  Verzeichniss  von  6323  telescopischen  Sternen,  +3°  bis 

+9°.     Munich,  1869.     8vo. 
:  Verzeichniss  von  3571   telescopischen  Sternen,  +9°  bis 

+15°.     Munich,  1871.     8vo. 
:  Verzeichniss  von  4093  telescopischen  Sternen,  — 9°  bis 

—15°.     Munich,  1872.     8vo. 
:  Verzeichniss  von  5563  teiescopischen  Sternen,  nbrdlich 

von  +15°,  und  sudlich  von  — 15°.     Munich,  1874.    8vo. 
:  Resultate  der  meteorologischen  Beobachtungen,  1825-66. 

Munich.     8vo. 

:  Sonnenfinsterniss  vom  18  Juli,  1860.    n.  p.,  n.  d.    8vo.    P. 

LANGLEY  (S.  P.):  On  the  minute  structure  of  the  Solar  photo- 
sphere.    New  Haven,  1874.     8vo.     P. 
:  On  the  comparison  of  certain  theories  of  Solar  structure 

with  observation.     New  Haven,  1875.     8vo.     P. 
:  Measurement  of  the  direct  effect  of  Sun  Spots  on  climates. 

London,  1876.     8vo.     P. 
:  On  the  possibility  of  transit  observation  without  personal 

error.     New  Haven,  1877.     8vo.     P. 
:  A  proposed  new  method  in   Solar  Spectrum  Analysis. 

New  Haven,  1877.     8vo.     P. 

:  Nouvelle  methode  Spectroscopique.    Paris,  1877.    4to.    P. 

:  Transit  of  Mercury,  1878.     New  Haven,  1878.     8vo.     P. 

:  Observations  on  Mt.  Etna.     New  Haven,  1880.     &vo.     P. 

:  Sur  la  distribution  de  1'energie  dans  le  spectre  solaire 

normal.     Paris,  1881.     4to.     P. 
:  Sunlight  and  skylight  at  high  altitudes.     New  Haven, 

1882.     8vo.     P. 

:  Observations  du  spectre  solaire.     Paris,  1882.     4to.     P. 

:  Observation  of  the  Transit  of  Venus,  1882.    London,  1883. 

8vo.     P. 


Lick  Observatory  Library.  61* 

LANGLEY  (S.  P.):  The  selective  absorption  of  solar  energy. 
New  Haven,  1883.  8vo.  P. 

:  Researches  on  Solar  Heat  (Mt.  Whitney  expedition). 

Washington,  1884.  4to. 

:  Experimental  determination  of  Wave  lengths  in  the 

invisible  prismatic  spectrum.  New  Haven,  1884.  8vo.  P. 

:  Observations  on  Invisible  Heat  Spectra,  etc.  New  Haven, 

1886.  8vo.  P. 

:  Sur  des  longueurs  d'onde  jusqu'ici  non  reconnues.  Paris, 

1886.  4to.  P. 

:  Sur  les  spectres  invisibles.     Paris  (1886).     8vo.     P. 

:  The  New  Astronomy.     Boston,  1888.     4to. 

:  Energy  and  Vision.     New  Haven,  1888.     8vo.     P. 

:  On  the  observation  of  sudden  phenomena.  New  Haven, 

1889.  8vo.  P.  Same.  Washington,  1889.  8vo.  P. 

:  The  temperature  of  the  Moon,  Third  Memoir.  Wash- 
ington, 1889.  4to.  P. 

:  See  HOLDEN. 

and  HOLDEN  (E.  S.):  First  Sketch  of  a  proposed  Solar 

Spectroscope  for  the  36-inch  Equatorial  of  the  Lick  Ob- 
servatory. 

,  YOUNG  (C.  A.),  and  PICKERING  (E.  C.):  PRITCHARD'S 

Wedge  Photometer.  Boston,  1886.  4to.  P. 

LAPLACE  (P.  S.  de) :  Mecanique  Celeste.  (Translated  by  N.  BOW- 
DITCH.)  Boston,  1829-39.  4to. 

:  Essai  philosophique  sur  les  probabilites.  6th  edition. 

Paris,  1840.  8vo. 

:  Oeuvres  de  LAPLACE.  Vols.  1,  2,  3,  4,  5,  6,  7,  bound  in  4 

vols.  Paris,  1843-47.  4to.  [Loaned  to  the  L.  O.  by 
GEORGE  F.  BECKER,  Ph.D.] 

LA  PLATA  (observatory):  Anuario,  1887-88-89-80.  Buenos 
Aires.  16mo. 

LASSELL  (W.):  On  polishing  the  Specula  of  Reflecting  Tele- 
scopes. London,  1875.  4to.  P. 

[LAUSSEDAT  (A.)]:  Notice  sur  les  Travaux  Scientifiques  de 
*  *  *  Paris,  1883.  4to.  P. 

:  Discours  aux  obseques  de  J.  B.  J.  D.  BOUSINGAULT. 

Paris,  1887.  8vo.  P. 

:  Sur  1'organization  de  plusieurs  Services  Scientifiques  aux 

Etats  unis — Astronomie.  Paris,  n.  d.  4to.  P. 


62*  Catalogue  of  the 


LEAVENWORTH  (F.  P.):  Micrometrical  measurements  of  Double 
Stars,  n.  p.  (1888).  8vo.  P. 

[LE  CONTE  (John)]:  See  STEVENS. 

LE  CONTE  (Joseph):  On  Some  Phenomena  of  Binocular  Vision. 
New  Haven,  1880.  8vo.  P. 

:  On  Some  Phenomena  of  Binocular  Vision,  XII.  New 

Haven,  1887.  8vo.  P. 

:  The  general  interior  condition  of  the  earth,  n.  p.,  1889. 

8vo.  P. 

LEDGER  (E.):  The  Sun;  its  Planets  and  their  Satellites.  Lon- 
don, 1882.  8vo. 

LEFROY  (J.  H.):  Diary  of  a  Magnetic  Survey  of  *  *  * 
Canada.  London,  1883.  8vo. 

LEHARDELAY    (C.):    Resultats   d'observations    de    la    planete 

Saturne  (1868-74).     Brussels,  1876.     8vo.     P. 
LEIDEN  (observatory):  Annalen.     Vols.  I,  II,  III,  IV,  V,  VI. 

Leiden.     4to. 
:  Catalogus  van  de  Boeken,   etc.,  in   de   Bibliothek   der 

Sterrenwacht  te  Leiden,  with  2  supplements.     The  Hague, 

1877-82.     8vo. 
:   Verslag,  etc.     1863-4;  1864-5;  1865-6;  1866-7;  1867-8; 

1868-9;  1869-70;  1870-1;  1871-2;  1872-3;  1873-4;  1874-5; 

1875-6;  1876-7;  1877-9;  1879-80;  1880-1;  1881-2;  1882--3; 

1883-4;    1884-5;   1885-6;    1886-8;   1888-9;   by  Professors 

KEYSER  and  v.  d.  S.  BAKHUYSEN.    Bound  in  1  vol.    Leyden, 

1864-89.     8vo. 
LEIPZIG  (Astronomische  Gesellschaft):  Publicationen  [entered 

under  the  names  of  the  separate  authors]  Vierteljahrsschrift 

1-2-3-4-5-6-7-8-9-10-11-12- 13-14-15-16-17-18-19-20- 

21-22-23-24.     Also,  Suppl.  I-II.     Leipzig,  1866.     8vo. 
LEIPZIG  (Royal  Saxon  Academy  of  Sciences):  Abhandlungen 

(der  Math.  Phys.  Classe).     Vol.  XIV  (parts  10, 11, 12, 13); 

XV  (3,  4,  5,  6).     Leipzig,  1888-9.     8vo. 

:  Berichte,  I,  1889.     Leipzig.     8vo. 

LE  MONNIER  (P.  Ch.):  Histoire  Celeste,  etc.     Paris,  1741.     4to. 
:  Observations  de  la  Lune,  du  Soleil  et  des  Etoiles  Fixes. 

3vols.     Paris,  1751-59.     folio. 
LENARD  (P.)  and  WOLF  (M.):  Zerstaeuben  der  Koerper  durch 

das  Ultraviolette  Licht.     Leipzig,  1889.     8vo.     P. 


Lick  Observatory  Library.  63* 

LEONHARD  (E.):  See  SEIDEL. 

LEONARD  (N.  E.):  Iowa  County  Meteor,  etc.     New  Haven,  1875. 

8vo.     P. 
LEVANDER  (F.  W.):  General  Index  to  the  first  20  vols.  of  the 

Astronomical  Register.     London,  1883.     8vo. 
LEVEAU  (G.):  See  LOEWY. 
LEWIS  (T.):  The  Greenwich  System  of    *    *    *    Time  Signals. 

London,  1885.     8vo.     P. 
LEYDEN  (observatory):  See  Leiden. 
LEYTON  (observatory):     See  BARCLAY. 
[LicK  (James)]:  Framed  diploma  of  Honorary  Membership  in 

La  Sociedad  Protectora  de  los  Animales  y  las  Plantas  de 

Cadiz.     Dated  July  1,  1874. 
[ ]:  Framed   diploma  of   the  Associazione  Internazionale 

d'Incoraggiamento,  conferring  the  title  of  Presidente  Onora- 

rio  Protettore,  with  medal.     Dated  Naples,  July  16, 1874. 
:  Deed  of  Trust  of  JAMES  LICK,  Esq.,  of  San   Francisco. 

Dated  September  21, 1875.     San  Francisco,  1875.    8vo.    P. 

[ ] :  Large  photographic  portrait,  colored  in  crayons. 

[ ]:  See  SPOOR. 

LINDEMANN  (E.) :  Zur  Beurtheilungder  Veraenderlichkeit  Rother 

Sterne.     St.  Petersburg,  1882.     folio. 
:  Helligkeitsmessungen  der  Bessel'schen  Plejaden  Sterne. 

St.  Petersburg,  1884.     folio. 
LINDSAY  (Lord):  Note  on  the  Spectrum  of  the  Red  Spot  on 

Jupiter,  etc.     London,  1879.     8vo.     P. 

:  See  Dun  Echt  (observatory). 

LINDSTEDT  (A.):  Ueber  die  Integration  einer  fiir  die  Storungs- 

theorie  wichtigen  Differentialgleichung.  Kiel,  1882.  4to.  P. 
:  Beitrag  zur  Integration  der  Differ entialgleichungen  der 

Stoerungstheorie.     St.  Petersburg,  1883.     folio.     P. 
[LIPPINCOTT  (S.  B.)]:  Gazetteer  of  the  World.     Philadelphia, 

1886.     8vo. 
LISBON   (Royal   Academy   of  Sciences):    Jornal.     (Nos.   1-8) 

(1866-69),  1  vol.;  (Nos.  23-32)  (1878-82),  1  vol.     Lisbon. 

8vo. 
LITTLE  (C.  N.):  On  Knots,  with  a  census  of  Ten.    (New  Haven  )r 

1885.     8vo.     P. 


64*  Catalogue  of  the 


LITTRE  (E.)  and  BEAUJEAN  (A.):  Dictionnaire  de  la  langue 
franchise.  Paris,  1883.  8vo. 

LITTROW  (C.  von):  Privatleistungen  auf  Astronomischen 
Gebiete.  Vienna,  1859.  8vo.  P. 

:  Andeutungen  ueber  Astronomische  Beobachtungen  bei 

totalen  Sonnenfinsternissen.  Vienna,  1860.  8vo.  P. 

:  Ueber  das  Zuriickbleiben  der  Alten  in  den  Naturwissen- 

schaften.  Vienna,  1869.  8vo.  P. 

LITTROW  (J.  J.):  Dioptrik  oder  Anleitung  zur  Verfertigung  der 
Fernrohre.  Vienna,  1830.  8vo. 

LIVERPOOL  (Astronomical  Society):  Journal.  Vols.  I,  II 
•  (1882-4);  Vol.  Ill  (parts  1-8);  Vol.  V  (parts  1,2,  3,  6,  7,  8); 
Vol.  VI  (1887-8);  Vol  VII  (parts  1-9).  Liverpool,  1882. 
Svo. 

LIVERPOOL  (Literary  and  Philosophical  Society):  Proceedings. 
Vols.  33  (1878-9),  34,  35,  36,  37,  38,  39,  40,  41,  42,  43. 
Liverpool.  Svo. 

LOCKE  (J.):  Observations  on  Terrestrial  Magnetism.  Wash- 
ington, Smithsonian  Institution.  4to.  P. 

[LOCKE  (R.  A.)]:  The  History  of  the  Moon,  or  an  account  of 
the  wonderful  discoveries  of  Sir  JOHN  HERSCHEL,  who,  by 
means  of  an  Object  Glass,  weighing  Seven  Tons,  with  a 
magnifying  power  of  42000  times,  has  been  enabled  to 
discover  in  the  MOON,  Rocks,  Trees,  Flowers,  Verdant 
Plains,  Volcanoes,  Lakes,  Seas,  Sheep,  Deer,  Bears,  and 
Beavers,  and,  more  wonderful  still,  intelligent  winged 
beings,  Male  and  Female,  who  fly  about  and  walk  erect  like 
men.  [The  Moon  Hoax  reprint.]  n.  p.  [London],  n.  d. 
[1836].  Svo. 

LOCKYER  (J.  N.):  Spectroscopic observations  of  the  Sun,  No.  II. 
London,  1868.  4to.  P. 

:  Researches  in  Spectrum  Analysis  in  Connexion  with 

the  Spectrum  of  the  Sun.  London,  1872.  4to.  P. 

:  Same.     No.  IV  (1874). 

:  Recent  researches  in  Solar  Chemistry.  London,  1878. 

8vo.  P. 

:  The  Chemistry  of  the  Sun.     London,  1887.     Svo. 

:  The  History  of  a  Star  (from  the  Nineteenth  Century). 

London,  1889.  Svo.  P. 


Lick  Observatory  Library.  65* 

LOCKYER  (J.  N.)  and  SCHUSTER  (A.):  Report  on  the  total  Solar 

Eclipse  of  April  6,  '1875.     London,  1878.     4to.     P. 
LOEW  (M.):  See  PLANTAMOUR. 
LOEWY  (B.):  See  DE  LA  RUE. 

LOEWY  (M.):  Determination  des  A.  R.  des  etoiles  de  culmina- 
tion lunaire,  etc.     Paris,  1886.     4to. 
:  Description  sommaire  d'un  nouveau  Systeme  d'equatori- 

aux,  etc.     Paris,  1888.     4to.     P. 
:  Deux  methodes  nouvelles  pour  de  la  determination  des 

R.  A.,  etc.     Paris,  1883.     4to.     P. 
:  Nouvelles  methodes  pour  la  determination  de  la  position 

relative   de   1'equateur    instrumental,    etc.      Paris,    1883. 

4to.     P. 
:  Etudes  di verses  sur  les  methodes  d'observation.  et  de 

reduction    des    observations    meridiennes.      Paris,    1885. 

4to.     P. 

:  Nouvelles  methodes  pour  la  determination  de  la  Refrac- 
tion.    Paris,  1886.     4to.     P. 
:  Nouvelles  methodes  pour  la  determination  de  la  con- 

stante  de  Faberration.     Paris,  1887.     4to.     P. 
:  Ephemerides  des  Etoiles  de  Culmination  lunaire,  etc.,  pour 

1883-86-87-88-89-90.     6  vols.     Paris.     4to.     P. 
:  Notice  Sur  la  Vie  et  les  travaux  de  M.  OPPOLZER.    Paris, 

8vo.     P. 
,  LEVEAU  (G.),  and  RENAN  (H.):  Etude  de  la  flexion  hori- 

zontale  de  la  lunette  du  Cercle  meridien,  etc.,  de  Paris. 

Paris,  1887.     4to.     P. 
and    PUISEUX  (V.):    Theories   nouvelles   de  Pequatorial 

coude.     Paris,  1888.     4to.     P.' 
and  TRESCA  (H.  E.) :  Notice  sur  un  nouvel  appareil  optique 

propre  a  1'etude  de  la  flexion.     Paris,  1882.     4to.     P. 
LOHRMANN  (W.  G.):    Topographic  der  Sichtbaren  Mondober- 

flaeche.     Leipzig,  1824.     4to. 
LOHSE  (0.):  Ueber  SCHMIDT'S  neuen  Stern  in  Schwan.     Berlin, 

1878.     8vo.     P. 
:  Star  Photography,  etc.,  Gelatine-Trockenplatten,  etc.     (5 

papers.)     London,  1881.     8vo.     P. 

:  Abbildungen   von   Sonnenflecken,  etc.     Potsdam,  1883. 

-     4to.     P. 


66*  Catalogue  of  the 


LOHSE(O.):  Ueber  Stellar  photographie.    Kiel,  1886.    4to.     P. 

:  Ueber  einige  Eigenschaften  der  Gelatine,  etc.  n.p.,n.  d. 

8vo.  P. 

:  See  VOGEL. 

LOMMEL  (E.):  JOSEPH  VON  FRAUNHOFER'S  Gesammelte  Schriften. 
Munich,  1888.  4to. 

:  G.  S.  OHM'S  wissenschaftliche  Leistungen.  Munich,  1889. 

4to.  P. 

LONDON  (British  Association  for  the  Advancement  of  Science): 
Reports,  183-  -2-3-4-7;  1841-2-3-4-5-6-7-8-9;  1851-2-3- 
4_5_6_7-8-9;  1860-1-2-3-4-5-6-7-8-9;  1870-1-2-3-4-6- 
7-8-9;  1880-1-2-3-4-5.  London,  1832.  8vo. 

LONDON  (B.  A.  A.  S.):  Report  (of  the  Montreal  meeting,  1884, 
from  "Science").  1vol.  Cambridge,  1884.  8vo. 

(The)  LONDON,  EDINBURGH,  AND  DUBLIN  PHILOSOPHICAL  MAGA- 
ZINE: Vol.  38  (1869),  Vol.  48  (1871),  bound  in  1  vol.  Also, 
Vol.  41  (1871).  London.  8vo. 

[LONDON  (Religious  Tract  Society)]:  The  Solar  System.  Lon- 
don, s.  d.  32mo. 

LONDON  (Royal  Astronomical  Society):  Memoirs.  Vols.  1  (1822); 
2,  3,  4,  5,  6,  7,  8,  9,  10,  11,  12,  13,  14,  15,  16,  17,18,  19,  20, 
21,  22,  23,  24,  25,  26,  27,  28,  29,  30,  31,  32,  33,  34,  35,  36, 
37  (i,  ii),  38,  39,  40,  41,  42,  43,  44,  45,  46,  47,  48,  49  (i,  ii). 
London,  1822.  4to. 

:  Monthly  Notices.  Vols.  1  (1827),  2,  -,  -,  -,  6,  7,  8,  9,  10, 

11,  12,  13,  14,  15,  16,  17,  18,  19,  20,  21,  22,  23,  24,  25,  26, 
27,  28,  29,  30,  31,  32,  33,  34,  35,  36,  37,  38,  39,  40,  41,  42X 
43,  44,  45,  46,  47,  48,  49,  50.  London,  1827.  8vo. 

:  Catalogue  of  the  Library,  R.  A.  S.     London,  1886.     8vo. 

:  List  of  Fellows.     London.     8vo.     P. 

:  A  General  Index  to  the  First  38  Volumes  of  the  Memoirs 

of  the  Royal  Astronomical  Society.  London,  1871.  8vo. 

:  See  Anonymous. 

LONDON  (Royal  Society):  Philosophical  Transactions.  BUTTON'S 
abridgment  to  1800,  18  vols.  Annual  volumes,  1801-71, 
inclusive;  Vol.  162,  Part  i  (1872).  Series  A:  1887-88- 
89.  London.  4to. 

:  Proceedings.  Vol.  31  (1880-81);  32,  33;  45,46,  47.  Lon- 
don. 8vo. 


Lick  Observatory  Library.  67* 

LONDON    (Royal    Society):     Catalogue    of    Scientific    Papers 
(1864-73).      Vols.   VII,   VIII.      [Temporarily   loaned   to 

the   Lick     Observatory   by    S.   W.   BURNHAM.]      London, 

1877.     4to. 

:   (List  of  Members.)     London.     4to.     P. 

:  See  Anonymous. 

LONDON  (Transit  of  Venus  Committee):  Report  (on  the  transit 

of  1882).     London,  n.  d.     folio.     P. 
LORENTZ  (E.):  See  SCHMTTZ. 
LONG  (R.):  Astronomy,  in  five  books.     2  vols.     Vol.  I  (1742); 

II  (1764).     Cambridge,  1785.     4to. 
[LooMis  (E.)]:  Life  of.     By  H.  A.  NEWTON.     New  Haven,  1890. 

8vo.     P. 
LORENZONI  (G.):  (Length  of  the  Seconds  Pendulum  at  Padua.) 

Rome,  1888.     4to.     P. 

LOVE  (J.):  Geodaesia.     13th  edition.     New  York,  1796.     12mo. 
LOVERING    (J.):    The   Mecanique  Celeste  of  LAPLACE,  and  its 

translation  by  BOWDITCH.     Boston,  1889.     8vo.     P. 
:  An  address  delivered   *   *    *   when  the  RUMFORD  medals 

were  presented  to  Professor  MICHELSON.     Boston.     8vo.     P. 
LUBBOCK  (J.  W.):  On  the  theory  of  the  Moon,  Part  X  (only). 

London,  1861.     8vo. 
LUTHER  {E.):  Declinationes  Stellarum  Fundamentalium  novae 

ex  ultimis  Illi.  BESSEL  observationibus  derivatse.     Koen- 

igsberg,  1859.     4to.     P. 
LUTHER  (W.):  Ueber  die  bahn  des  planeten  Amalthea.    Leipzig, 

1883.     8vo.     P. 

LYME-REGIS  (Rousdori  Observatory):  Publications. 
LYONS  (observatory):   Travaux.     Vol.  I.     Lyons,  1888.     4to. 
MADAGASCAR  (Royal  Observatory):  Resume  des  observations 

meteorologiques    faites   a   Tananarive.      [Transferred    to 

University  Library,  Berkeley.]    Tananarive,  1890.    8vo.    P. 
MADISON (Washburn  Observatory):   Contributions,  No.  1 .    Madi- 
son, 1881.     4to.     P. 

:  Publications.    Vols.  1,  2,  3,  4,  5.     Madison,  1881.     8vo. 

[ ] :  Framed  wood-cut  of. 

MADISON  (Wisconsin  Academy  of  Sciences):  Transactions.    Vol. 
VI  (1881-3).     Madison.     8vo. 


68*  Catalogue  of  the 


MADRAS  (observatory):  Results  of  Observations  of  the  Fixed 
Stars  with  the  Meridian  Circle  in  1862-3-4  (1  vol.);  1865- 
6-7  (1  vol.).  Madras,  1887-8.  4to. 

:  See  POGSOX. 

MADRID:  Almanaque  Nautico.  [Transferred  to  the  University 
Library,  Berkeley.] 

MADRID  (Royal  Observatory):  Anuario.  [Transferred  to  the 
University  Library,  Berkeley.] 

MAEDLER  (J.  H.):  Kurzgefasste  Beschreibung  des  Mondes.  Ber- 
lin, 1839.  8vo. 

:  Die  Eigenbewegungen  der  Fixsterne,  etc.  [Dorpat  Ob- 
servations, Vol.  XIV.]  Dorpat,  1856.  4to. 

:  See  BEER  and  MAEDLER. 

:  See  Dorpat. 

MAGNAC  (A.  de):  Recherches  sur  Pemploi  des  Chronometres  a 
la  Mer.  Paris,  1874.  8vo.  P. 

MAGNAC  (H.  de):  Le  navisphere.     Paris,  1879.     8vo.     P. 

MAILLY  (E.):  Precis  de  1'histoire  de  PAstronomie.  Brussels, 
1860.  16mo. 

MAIN  (R.):  MASKELYNE'S  Ledgers  of  Stars.  (Appendix  II, 
Greenwich  Obs.,  1851.)  London,  1853.  4to. 

:  Second  Radcliffe  Catalogue  of  2386  Stars.  Oxford,  1870. 

8vo. 

:  See  HERSCHEL.     See  Oxford. 

MAIRAN  (J.  J.  d'O.  de):  Traite  de  1'Aurore  Bore'ale.  Paris, 
1733.  4to. 

MAKENAUER  (E.):  Kometen  und  Sonnenlicht.  Vienna,  1865. 
16mo.  P. 

MANCHESTER  (Literary  and  Philosophical  Society):  Memoirs  and 
Proceedings,  1887-9.  1  vol.  Manchester.  8vo. 

MANNHEIM:  Astronomische  Beobachtungen  auf  der  *  *  * 
Sternwarte  zu  Mannheim.  I.  Abtheilung  (E.  SCHOENFELD), 
1862.  II.  Abtheilung  (E.  SCHOENFELD),  1875.  III.  Ab- 
theilung (W.  VALENTINER),  1879.  Mannheim.  4to. 

MANNHEIM  (observatory):  See  Karlsruhe. 

MARCUSE  (A.):  Ableitung  der  R.  A.  der  Sterne  des  Fundamental- 
Cataloges  der  Ast.  Gesell.  aus  den  von  H.  ROMBERG  (1869-73) 
am  grosseren  Meridian  Instrumente  der  Berliner  Stern- 
warte angestellten  Beobachtungen.  Berlin,  1888.  4to.  P. 


Lick  Observatory  Library.  69* 

MARTH  (A.):   On  the  formulae  for  correcting  approximate  ele- 
ments of  the  orbits  of  binary  Stars.    London,  1887.    8vo.    P. 
:  On  the  formulae  for  computing  the  apparent  positions  of 

a  satellite,  etc.     London,  n.  d.     8vo.     P. 
:  [Ephemerides  of  the  Moon,  Planets,  and  Satellites,  1880— 

90.]     23  numbers  bound  in  1  vol.     London.     8vo. 
:  Data  for  a  graphic  representation  of  the  Solar  System. 

London,  n.  d.     8vo.     P. 
MARTIN  (P.):  The  Statesman's  Yearbook.     3  vols.,  1878-79-80. 

London,  1878-80.     8vo. 
MASKELYNE  (N.):  See  MAIN. 

[MASON  (E.  P.)]:  Life  of,  by  D.OLMSTED.    New  York,  1842.    8vo. 
MAUPERTUIS  (Ch.):  Oeuvres.     4  vols.     Lyons,  1756.     8vo. 
MAURY  (M.   P.):   The.  Physical  Geography  of  the  Sea.     New 

York,  1858.     8vo. 
MAXWELL  (J.  C.):  Theory  of  Heat.    8th  edition.    London,  1885. 

16mo. 
:  The  Scientific  Papers  of  JAMES  CLERK  MAXWELL,  edited 

by  W.  D.  NIVEN.     2  vols.     Cambridge,  1890.     4to. 
MAYER  (A.M.):  Observations  on  the  planet  Jupiter  (from  Jour* 

Frank.  Inst.).     Philadelphia,  1870.     8vo.     P. 
MAYER  (T.):  TOBIAS  MAYER'S  groessere  Mondkarte,  etc.  (bound 

in  1  vol.).     Gottingen,  1881.     folio. 
:  TOBIAS   MAYER'S  groessere  Mondkarte,4  framed  plate  of 

the  full  Moon. 

McLEOD  (C.  H.):  Report  of  the  Canadian  observations  of  the 

Transit  of  Venus,  1882.     n.  p.,  n.  d.     8vo.     P. 

:  See  ROGERS. 

MCCLINTOCK  (Sir  F.  L.):    Meteorological  Observations  in  the 

Arctic  Seas  in  1857-58-59.      Reduced   by  C.  A.  SCHOTT. 

Washington,  Smithsonian  Institution,  1862.     4to.     P. 
MCCLURE  (E.):  See  KLEIN. 
MECHANICAL  NEWS:   [Transferred   to  the   University  Libraryr 

Berkeley.]     New  York.     4to. 
MEIER  (J.):  See  NEWCOMB. 
MELANGES  Mathematiques  et  Astronomiques:  Vols.  1,  2,  3,  4,, 

5,  6  (i,  ii,  iii).     St.  Petersburg,  1853.     8vo. 


70*  Catalogue  of  the 


MELBOURNE    (observatory):    First   general   catalogue   of  1227 

Stars.     1870.0.     Second,   1880.0.     Melbourne,    1874.     4to. 
:  Results  of  Astronomical  Observations  (1876-7-8-9-80),  1 

vol.;  (1881-2-3-4),  1vol.    Melbourne,  1884 and  1888.    8vo. 
:  Observations  of  the  Southern  Nebulae  (1869-1885),  Part 

I.     n.  p.,  n.  d.     folio. 

:  Monthly  Record  of  Results  of  Observations  in  Meteor- 
ology, etc.     [Transferred  to  University  Library,  Berkeley.] 
MENDENHALL  (T.  C.):  On  the  intensity  of  earthquakes.     Salem, 

1888.     8vo.     P. 
MEUDON    (observatory):     Communications    a   1' Academic   des 

Sciences  de  Paris,  1880.  1881,  1882.     Paris.     4to.     P. 
MERIDEN    (Scientific    Association):     Transactions.       Vol.    IV 

(1889-90).      [Transferred    to    the     University     Library, 

Berkeley.]     Meriden,  189,1.     8vo.     P. 
MERRIMAN  (M.):  A  text-book  on  the  Method  of  Least  Squares. 

New  York,  1888.     8vo. 
MESSERSCHMTTT    (J.    B.):    Ueber   diffuse   Reflexion.     Leipzig, 

1888.     8vo.     P. 
MEXICO    (Sociedad   Cien tinea  "Antonio  Alzate"):   Memoirs  y 

Revista.     Tome  IV  (1890),  current.     Mexico.     8vo.     P. 
MEYER  (M.  W.):  Von  der  Erde  bis  zum  Monde.     Berlin,  1889. 

8vo.     P. 
MICHELSON    (A.  A.):    A  plea   for  light  waves.     Salem,  1888. 

8vo.     P. 
:  Measurement  of  Light  Waves.     New  Haven,  Feb.,  1890. 

8vo.     P. 
:  A  simple  interference  experiment.     New  Haven,  March, 

1890.     8vo.     P. 
and  MORLEY  (E.  W.):  On  the  feasibility  of  establishing 

a  light  wave  as  the  ultimate   standard  of  length.     New 

Haven,  1889.     8vo.     P. 

MILAN  (Royal  Observatory):  Pubblicazioni  del  R.  Osservatorio 
di  Brera  (in  quarto). 

I.  G.  CELOBIA  :  Sul  grande  commovimento  atmosferico  avvenuto  il  1.° 
di  Agosto  1872  nella  Bassa  Lombardia  e  nella  Lomellina.  pag.  12  con  una 
tavola  litografica.  (1873.)  — II.  G.  V.  SCHIAPABELLI:  Osservazioni 


Lick  Observatory  Library.  71* 

MILAN  (Royal  Observatory): 

astronomische  e  fisiche  sulla  gran  cometa  del  1862.  pag.  38  con  5  tavole 
litografiche.  (1873.)  —  III.  G.  V.  SCHIAPARELLI:  I  precursor! di  Copernico 
nell'aiitichita.  pag.  52.  (1873.)  —  IV.  G.  CELOEIA:  Variazioni  perio- 
diche  e  non  periodiche  della  temperatura  nel  clima  di  Milano.  pag.  86 
con  3  tavole  litografiche.  (1874.)  —  V.  G.  TEMPEL:  Osservazioni  astro- 
nomiche  diverse  fatte  nella  Specola  di  Milano  negli  anni  1871  a  1874. 
pag.  20  con  3  tavole  fotografiche  rappresentanti  la  cometa  di  Coggia,  una 
carta  delle  Plejadi,  e  2  tavole  litografiche.  (1874.)  —  VI.  G.  PIA/ZI  e  B. 
ORIANI:  Corrispondenza  astronomica.  pag.  204.  (1875.)  [Bound  in  1 
vol.] 

VII.  (Partel.a):  Osservazioni  di  stelle  candenti  fatte  nelle  stazioni 
.italiane  durante  gli  anni  1868,  1869,  e  1870.  pag.  100.  (1882.)  —  (Parte 
2.a):  Id.  durante  1'anno,  1871.  pag.  116.  (1885.)  —  (Parte  3.*):  Id. 
durante  1'anno  1872.  pag.  84.  (1874.)  —  VIII.  G.  V.  SCHIAPARELLI  e 
G.  CELORIA:  Determinazione  (1870)  della  differenza  di  longitudine  dell' 
Osservatorio  di  Milano  coll'Osservatorio  de  Neuchatel  e  con  la  stazione 
trigonometrica  del  Sempione.  pag.  46.  (1875.)  —  IX.  G.  V.  SCHIAPA- 
RELLI: Le  sfere  omocentriche  di  Eudosso,  di  Callippo  e  di  Aristotele. 
pag.  64  con  2  tavole  litografiche.  (1875.)  —  X.  G.  CELORIA:  Sull'eclissi 
sola,re  totale  del  3  Giugno  1239.  pag.  26  con  una  tavola  litografica. 
(1875).  —  XI.  G.  CELORIA  :  Sugli  eclissi  solari  totali  del  3  Giugno  1239  e 
del  6  Ottobre  1241.  pag.  20  con  2  tavole  litografiche.  (1876.)  — XII.  P. 
FRISIANI  :  Su  alcuni  temporal!  osservati  nell'  Italia  superiore  (estate 
1876).  pag.  20  con  3  tavole  litografiche.  (1877.)  [Bound  in  1  vol.] 

XIII.  G.  CELORIA  :  Sopra  alcuni  scandagli  del  cielo  eseguiti  alPOsser- 
vatorio  Real  di  Milano.  pag.  48  con  5  tavole  litografiche.  (1878.)  —  XIV. 
G.  CELORIA  e  G.  LORENZONI  :  Determinazione  (1875)  delle  differenze  di 
longitudine  fra  gli  Osservatorii  astronomici  di  Milano  e  di  Padova  e 
quelli  di  Vienna  e  di  Monaco  (di^Baviera).  pag.  82  con  una  tavola  incisa 
in  legno.  (1879.)  — XV.  G..  V.  SCHIAPARELLI:  Sull'  umidita  atmos- 
f erica  nel  clima  di  Milano.  Risultati  di  35  anni  di  Osservazioni  fatte 
nell' Osservatorio  di  Brera  (1845-79).  pag.  36  con  3  tavole  litografiche. 
(1880.)  — XVI.  G.  V.  SCHIAPARELLI  e  P.  FRTSIANI:  Sui  temporali 
osservati  nell'  Italia  superiore  durante  1'anno  1877.  pag.  90  con  5  tavole 
colorate  e  13  nere.  (1880.)  —  XVII.  G.  V.  SCHIAPARELLI,  P.  FRISIANI, 
ed  E.  PINI  :  Id.  durante  1'anno  1878.  pag.  100  con  8  tavole  litografiche. 
(1884.)  — XVIII.  E.PiNi:  Id.  durante  1'anno  1879.  pag.  150  con  7  tavole 
nere  e  8  colorate.  (1885.)  [Bound  in  1  vol.] 

XIX.  M.  RAJNA:  Determinazione  (1880-81)  della  latitudine  dell' 
Osservatorio  di  Brera  in  Milano  e  dell'  Osservatorio  della  R.  Universita 
in  Parma,  pag.  22.  (1881.) — XX.  C.  FORNIONI:  Osservazioni  mete- 
orologiche  orarie  ottenute  da  strumenti  registratori  nel  1880.  pag.  54 
con  5  tavole  litografiche.  (1882.)  —  XXI.  G.  CELORIA  e  L.  RESPIGHI: 
Determinazione  (1879)  della  differenza  di  longitudine  tra  gli  Osservatorii 
astronomici  di  Brera  in  Milano  e  del  Campidoglio  in  Roma.  pag.  68 
con  una  incisione  in  legno.  (1882.)  —  XXII.  A.  VENTURI:  Metodo  di 
Hansen  per  calcolare  le  perturbazioni  dei  piccoli  pianeti.  pag.  122. 
(1882.)  —  XXIII.  C.  FORNIONI:  Osservazioni  meteorologiche  orarie 
ottenute  da  strumenti  registratori  nel  1881.  pag.  56  con  6  tavole  lito- 
grafiche. (1883.)  — XXIV.  G.  CELORIA,  G.  LORENZONI,  e  A.  NOBILE: 
Determinazione  (1875)  delle  differenze  di  longitudine  tra  gli  Osservatorii 

13 


72*  Catalogue  of  the 


MILAN  (Royal  Observatory): 

astronomic!  di  Milano,  Padova,   Napoli  e  Genova.     pag.  128.    (1883.) 
[Bound  in  1  vol.] 

XXV.  L.  BILLOTTI:  Teoria  degli  strumenti  ottici,  con  applicazioni 
ai  telescopi  ed  alia  fotografia  celeste,  pag.  238  con  7  tavole  litogranche. 
(1883.)  —  XXVI.  M.  RAJNA:  Sulle  variazioni  diurne  del  magnetismo 
terrestre  a  Milano  negli  anni  1872  e  1877.  pag.  60  eon  8  tavole  litogra- 
fiche.  (1884.)  —  XXVII.  C.  FORNIONI:  Osservazioni  meteorologiche 
orarie  ottenute  da  strumenti  registratori  nel  1882.  pag.  56  con  6  tavole 
litogranche.  (1885.)  —  XXVIII.  A.  VENTURI:  Di  una  notevole  sempli- 
ficazione  nel  calcolo  delle  perturbazioni  dei  piccoli  pianeti.  pag.  16. 
(1886.)  — XXIX.  G.  CELORIA:  Determinazione  (1881)  delle  differenze 
di  longitudine  tra  Milano,  Nizza  e  Parigi.  pag.  96.  (1887.)  —  XXX.  F. 
PORRO  :  Determinazione  (1885)  della  latitudine  di  Termoli.  pag.  34. 
(1887.)  --  XXXI.  M.  RAJNA  :  Azimut  assoluto  (1882)  del  segnale  trigo- 
nometrico  del  Monte  Palanzone  sulP  orizzonte  di  Milano.  pag.  128. 
(1887.)  —  XXXII.  F.  BORLETTI:  Nuova  triangolazione  della  citta  di 
Milano.  pag.  16  con  4  tavole  litografiche.  (1887.)  —  XXXIII.  G.  V. 
SCHIAPARELLI  :  Osservaziom  sulle  stelle  doppie.  Serie  prima,  com- 
prendente  le  misure  di  465  sistemi  eseguite  col.  Refrattore  di  8  pollici  di 
Merz  negli  anni  1875-85.  pag.  148  con  2  tavole  litogranche.  (1888.)  — 
XXXIV.  G.  V.  SCHIAPARELLI:  Sulla  distribuzione  apparente  delle 
stelle  visibili  ad  occhio  nudo.  pag.  32  con  8  tavole  cromolitografiche. 
(1889.)  —  XXXV.  M.  RAJNA:  Confront!  e  verificazioni  d'azimut  asso- 
luti  in  Milano,  con  alcune  notizie  sulle  antiche  triangolazioni  nei  din- 
torni  di  questa  citta.  pag.  56  con  5  incisioni  intercalate  nel  testo.. 
).)  [Bound  in  1  vol.,  except  No.  33.] 


MILL  (H.  R.):  The  Rain  band,  etc.     London,  1883.     8vo.     P. 
MILLER   (W.   A.):    Introduction   to   the    study   of    Inorganic 

Chemistry.     London,  1873.     16mo. 
MILLOSEVICH  (E.):  Annotazioni  di  C.  H.  F.  PETERS  alia  Revis- 

ione  delle  "Anonymous  Boreali"  del  catalogo  di  YARNALL. 

Rome,  1885.     folio.     P. 
MILNE  (J.):  Earthquakes.     New  York,  1886.     8vo. 

MIRINNY  (L.):  Note  a  propos  des  "Canaux"  de  Mars.     Paris,. 

1888.     16mo.     P. 

:  *     *     *     L'heliogenese,  etc.     Paris,  1889.     32mo.     P. 

[MITCHELL   (0.   M.)]:    Sketch   of  (his   life)    (from  Pop.  ScL 

Monthly).     New  York,  1884.     8vo.     P. 
MODENA  (observatory):  Atti  del  R.  Osservatorio  Astronomico 

di  Modena.     Raccolti  e  ordinati  da  G.  BIANCHI.     Vol.  L 

Modena,  1834.     folio. 
MOEBIUS  (A.  F.):  Die  Elemente  der  Mechanik  des  Himmels. 

Leipzig,  1843.     8vo. 


Lick  Observatory  Library.  73* 

MOELLER    (A.):    Undersokning   af  Fayeska   Kometens   Bana. 

Stockholm,  1862.     4to. 
:  Nya  Elementer  for  Pandora,  etc.     1858-77.     Stockholm, 

1879.     8vo.     P. 
MONATLICHE  CoRRESPONDENz  i  Vols.  1-28  and  Register.     Gotha, 

1800-13.     8vo. 
MONCARLIERI   (R.  Collegio  Carlo  Alberto):  Bolletino  decadico. 

Bolletino  mensuale.     [Transferred  to  University  Library, 

Berkeley.] 

MONCK  (W.  H.  S.):  The  distributions  of  stars  in  space.     (Re- 
printed from  Proc.  R.  Dub.  Soc.)     Dublin,  18§5.     8vo. 
:  On  the  inclinations  of  Cometary  orbits.     London,  1887. 

8vo.     P. 
:  A    Catalogue   of  the  Aphelia   of  Comets,     n.  p.,  n.  d. 

Svo.     P. 
MONTESSUS  (F.  de):  Etude  sur  la  repartition  horaire  diurne- 

nocturne  des  seismes,  etc.   (two  parts;  one  from  Archives 

des  Sciences,  Vol.  22,  and  one  lithographed  ms.).     Geneva, 

1889.     8vo  and  folio.     P. 
MONTSOURIS    (observatory):     Annuaire   for   1884,   1885,    1886. 

Paris.     32mo. 
MORGAN  (A.  de):  The  Differential  and  Integral  Calculus.     Part 

I  only  (32  pp.).     S.  D.  U.  K.     London,  1836.     Svo.     P. 
MORTON  (E.  J.  C.):  Heroes  of  Science — Astronomers.     London, 

n.  d.     Svo. 
Moscow  (University  observatory):  Annales.    IX,  X  (1883-84), 

bound  in  1  vol.     New  Series  1  (1886-88).     Moscow.     4to. 
MOUCHEZ   (E.):  Catalogue  de  1'Observatoire  de  Paris,  Vol.  1; 

0  to  VI  hours.     Paris,  1887.     4to.     P. 
MOUNT   HAMILTON    (Lick   Observatory):    Publications,  Vol.   I. 

Sacramento,  1887.     4to. 
:  Suggestions  for  observing  the  Total  Eclipse  of  the  Sun 

on  January  1,  1889.     Sacramento,  1889.     Svo.     P. 
r-:  Reports  on  the  Total  Eclipse  of  the  Sun,  Jan.  1,  1889. 

Sacramento,  1889.     Svo. 
:  Reports  on  the  observations  of  the  Total  Eclipse  of  the 

Sun,  December  21-22,  1889,  etc.     Sacramento,  1891.     Svo. 


74*  Catalogue  of  the 


MOUNT  HAMILTON  (Lick  Observatory):  Observing  List  of  all 
B.  J.  Stars,  visible  at  L.  O.,  arranged  in  order  of  R.  A.  for 
1890  (including  transits  of  Stars  S.  P.),  with  settings  in 
Z.  D.  in  two  parts.  Part  I,  Clamp  W;  Part  II,  Clamp  E; 
compiled  by  G.  C.  COMSTOCK.  Ms.  1885.  4to. 

:  Ms.  and   other   accounts   of  earthquakes   in    California 

from  Oct.  21,  1868,  onwards,  chronologically  arranged. 

:  Ms.  reports  on  the  Solar   Eclipse  of  January   1,  1889, 

alphabetically  arranged. 

:  List  of  Addresses  of  Scientific  Societies,  Observatories, 

and  Astronomers  who  receive  the  Publications  of  the  LICK 
Observatory.  Ms. 

:  Visitors'  Book.     1.  From  1885,  July  6,  to  1888,  June  1. 

2.  From  1888,  June  1,  to  1890,  July  28.  3.  From  1890, 
July  28,  to  date.  3  vols.  Ms.  folio. 

:  Ms.  daily  record  of  the  depth  of  water  in  the  four  reser- 
voirs from  June  1,  1888,  to  date;  kept  by  E.  S.  HOLDEN 
and  E.  C.  HOLDEN.  Ms.  4to. 

:  Album  of  complete  set  of  blue  prints  of  the  plans  of  the 

75-foot  Dome;  reduced  to  8x10  inches  from  the  originals  of 
the  Union  Iron  Works. 

:  Scrap  Books,  relating  to:  Vol.  I,  Meridian  Instruments; 

II,  Equator ials;  III,  Clocks;  IV,  Time  Service;  V,  Circu- 
lars; Buildings;  Water  Supply;  Miscellaneous. 

:  Scrap  Book  containing  Astronomical  Telegrams  sent  and 

received  from  1888,  June  1,  to  date.     Ms.     4to. 

:  Scrap  Books  relating  to;  History  L.  O.     1  vol.     Official 

action  of  the  U.  S.;  of  the  State  of  California;  of  the 
Regents  of  the  University;  of  the  Director  of  the  Observa- 
tory, etc.  2  vols. 

:  Scrap  Books  relating  to;  Drawings  and  photographs  of 

the  Sun,  Moon,  Planets,  etc.  1  vol.  Photographs  of  Astro- 
nomical Instruments.  1  vol.  Proofs  of  electrotypes  owned 
by  the  L.  0.  1  vol. 

:  Scrap  Book  relating  to  The  Solar  eclipses  of  Jan.  1, 1889, 

and  Dec.  21,  1889.     1  vol. 

:  Portfolio  of  full  set  of  blue  prints  relating  to  the  36-inch 

equatorial;  presented  by  WARNER  &  SWASEY. 
Portfolio  of  Drawings  and  large  photographs  of  the. Moon. 


:  Portfolio  of  detached  maps. 


Lick  Observatory  Library.  75* 

MOUNT  HAMILTON  (Lick  Observatory):  Frame  of  views  of  L. 

0.  from  negatives  by  H.  E.  MATHEWS. 

[ ] :  Framed  map  of  Townships  6  and  7,  near  Mt.  Hamilton. 

[ ] :  Framed  map  of  parts  of  Townships  6  and  7,  near  Mt. 

Hamilton,  showing  Rain  Gauge  stations  of  S.  V.  W.  W. 
[ ]:  Framed  map  of  the  Reservation — scale,  40  chains  to  1 

inch. 
[ ]:  Framed  map — The  Public  Lands  of  San  Jose  (July, 

1886). 
[ ]:  Framed  photograph  of  the  summit  of  Mt.  Hamilton, 

1877. 

:  See  Berkeley. 

:  See  TODD,  D.  P. 

MULLER  (F.):  Definitive   determination   of  Comet,  1887,  IV. 

Cambridge,  n.  d.     4to.     P. 
MUNICH  (Academy   of  Sciences):    Sitzungsberichte,  1889-1890 

(current).     Munich.     8vo. 
MUNICH    (observatory):      Annalen    (1-2)    (1848-9),    (3-4-5), 

(6-7-8),  (9-10-11),  (12-13-14),  (15-16),  (17-18),  (19-20- 

21).     Munich,  1848-76.     8vo. 
:   Observationes  astronomies  (1-2-3)  (1820-24),  (4-5-6-7), 

(8-9-10-11),  (12-13-14-15).     Munich,  1820-44.    4to. 
:   Annalen.     Supplement  bande;  vols.  4-10-14,  bound  in 

1  vol.     Munich.     8vo. 
:  Meteorologische    Beobachtungen,    1825-37    and    1876-82, 

bound  in  1  vol.     Munich.     8vo. 
:  Annalen  fuer  Meteorologie.    (1-2-3-4)  (1842),  (5-6-7-8) 

(1843),  (9-10-11-12)  1844.     Munich.     8vo. 

:  Jahresbericht,  1852-54-58,  1  vol.     Munich.     8vo. 

= :  Jahrbuch  for  1838-39-40-41,  bound  in  1  vol.     Munich. 

16mo. 
:  Beobachtungen  auf  dem  Hohenspeissenberg,  1792-1850. 

Munich,  1851.     8vo. 
:  Neue    Annalen    der    K.    Sternwarte.      Band   I    (1890). 

Erstes  Muenchener  Stern  Verzeichniss    *    *    *    von  33082 

Sternen.     Munich,  1890.     4to. 
MONTSOURIS   (observatory):  Annuaire,  1888-89,  1  vol.     Paris. 

16mo. 
NATAL  (observatory):  Report  for  1888;  for  1889.     Pietermaritz- 

burg.     folio.     P. 


76*  Catalogue  of  the 


(The)  NATIONAL  ALMANAC  AND  ANNUAL  RECORD  FOR  1863. 
Philadelphia,  1863.  8vo. 

NATURE:  Vols.  5-6-7-8-9,  10-11-12-13-16-19,  20-1-2-3-4-5- 
6-7-8-9,  30-1-2-3-5-6-7-8-9,  40,  41,  42  (current).  Lon- 
don, 1871-  8vo. 

NATURE  NOVITATES:  (1880-1-2-3),!  vol.;  (1884-5-6-7),!  vol.; 
1888-9,  not  bound.  The  series  is  not  entirely  complete. 
Berlin.  8vo. 

NAUTICAL     ALMANAC  :     1840-2-4-6-7-8-9,    1 850-1-2-3-4-5-6, 

1862,  1879,  1880-1-3-4-5-6-7-8-9,  1890-1-2-3.     London. 

8vo. 
NEGRETTI    AND    ZAMBRA:    Encyclopaedic     *     *     *     Catalogue 

Of    *     *     *     Instruments.     London,  n.  d.     8vo. 
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:  On  the  Corrections  to  HANSEN'S   Tables  of  the  Moon. 

London,  1885.     4to.     P. 
NETOLICZKA  (E.):  Wie  sieht  es  auf  dem  Monde  aus?     Vienna, 

1867.     8vo.     P. 

NEUCHATEL  (observatory):  Rapport,  1887.     Locle.     8vo.     P. 
NEUMAN  &  BARETTI:  See  Dictionary. 
NEVADA  STATE  WEATHER  SERVICE:  See  Carson. 
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:  On  the  general  integrals  of  planetary  motion.     Wash- 
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Moon.     Washington,  1876.     4to.     P. 
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[in  America],     n.  p.,  1876.     8vo.     P. 
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Moon,  with  tables,  etc.     Washington,  1876.     4to.     P. 


Lick  Observatory  Library.  77* 

NEWCOMB  (S.):  Mean  motion  of  the  Moon   (from  Amer.  Jour. 

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:  Instructions  for  observing  the  Transit  of  Mercury,  1878. 

Washington,  1878.     4to.     P. 

:  Popular  Astronomy.     New  York,  1878.     Svo. 

:  Tables  of  Eclipses.     Washington,  1879.     4to. 

:  Populaere   Astronomic   von    SIM.    NEWCOMB.     Deutsche 

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:  Discussion    of    observations    on    Transits   of    Mercury, 

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:  On  the  motion  of  Hyperion.     Washington,  1884.     4to.    P. 

:  Measures  of  the  Velocity  of  light  made     *     *     *     (in) 

1880-82.     Washington,  1885.     4to.     P. 

:  Principles  of  Political  Economy.     New  York,  1886.     Svo. 

(Secretary):  Papers  relating  to  the  Transit  of  Venus  in 

1874,  prepared     *     *     *     by  the  Commission  authorized 

by  Congress.     Part  I,  Part  II.     Washington.     4to. 

:  See  Washington  (American  Ephemeris). 

:  See  Washington  (U.  S.  Naval  Observatory). 

:  See  Washington  (U.  S.  Transit  of  Venus  Commission). 

and  HOLDEN  (E.  S.):  On  the  possible  periodic  changes  of 

the  Sun's  apparent  diameter.     New  Haven,  1874.     Svo.    P. 
and   MEIER    (J.):    Transformation    of    HANSEN'S    Lunar 

Theory.     Washington,  1880.     4to.     P. 
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New  Haven.     4to. 
:  Report   for   the   year   1884-5,   1885-6,    1886-7,    1887-8, 

1888-9.     5  numbers.     New  Haven.     Svo.     P. 
NEWMARK  (N.):  The  Political  Code  of    *     *     California.     San 

Francisco,  1881.     16mo. 
NEWTON  (H.)  and  JENNEY  (W.  P.):  *     *  Geology  and  resources 

of  the  Black  Hills,  etc.     Washington,  1880.     4to. 
NEWTON  (H.  A.):  Explanation  of  the  motion  of  the  Gyroscope. 

New  Haven,  1857.     Svo.     P. 
:  On   the   meteor   of  November   15,   1859.     New   Haven, 

1860.     Svo.     P. 
:  Two  Meteoric  Fire  Balls  observed   (in)   August,  1860. 

New  Haven,  1862.     Svo.     P. 


78*  Catalogue  of  the 


NEWTON  (H.  A.):  Procession  and  periodicity  of  the  November 
Star  Shower,  etc.  New  Haven,  1863.  8vo.  P. 

Shooting  Stars  on  the  night  of  November  13-14,  1863. 
New  Haven,  1864.  8vo.  P. 

On  November  Star  Showers.    New  Haven,  1864.    8vo.    P. 

Altitudes  of  Shooting  Stars.    New  Haven,  1864.    8vo.    P. 

Abstract  of  a  memoir  on  Shooting  Stars.     New  Haven, 

1865.  Svo.     P. 

Altitudes  of  Shooting  Stars,  November  13-1 4, 1863.  New 
Haven,  1865.  Svo.  P. 

The  relative  number  of  Shooting  Stars  seen  in  a  given 
period  by  different  numbers  of  observers.  New  Haven, 

1866.  Svo.     P. 

:  November  meteors  in  1866.     New  Haven,  1867.     Svo.     P. 

:  Shooting  Stars  in  November,  1866.     New  Haven,  1867. 

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:  On   certain   recent   contributions  to  Astro-Meteorology. 

New  Haven,  1867.     Svo.     P. 
:  Meteors   of    November    14,    1868.      New   Haven,   1868. 

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:  Evidence  of  the  Cosmical  Origin  of  Shooting  Stars,  etc. 

New  Haven,  1868.     Svo.     P. 
[ ]:  Shooting  Stars  of  November  14,  1867.     New  Haven, 

1868.     Svo.     P. 
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1868.     Svo.     P. 
:  The  metric  system     *     *     *     with  tables.    Washington  r 

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Svo.     P. 

:  Meteors  of  November,  1869.     New  Haven,  1870.     Svo.    P. 

:  Observations  upon  the  meteors  of  November  24-27, 1872. 

New  Haven,  1873.     Svo.     P. 
:  An  Address  before  the  A.  A.  A.  S.,  1875.     Salem,  1875. 

Svo.     P. 

:  Meteor  of  December  21, 1876.  New  Haven,  1877.   Svo.    P. 

:  On  the  effect  upon  the  earth's  velocity  produced  by  small 

bodies  passing  near  the  earth.     New  Haven,  1885.    Svo.    P. 
:  The  story  of  Biela's  Comet.     New  Haven,  1886.     Svo.    P. 


Lick  Observatory  Library.  79* 

NEWTON  (H.  A.):    The  Biela  meteors  of  November  27,  1885. 

New  Haven,  1886.     8vo.     P. 
:  The   Meteorites,  the   Meteors,  and  the  Shooting  Stars. 

Salem,  1886.     8vo.     P.  .  ?  / 
:  Upon   the   relation   which   the   former   Orbits  of  those 

Meteorites  that  are  in  our  collections,  and  that  were  seen  to 

fall,  had  to  the  Earth's  orbit.     New  Haven,  1888.     8vo.     P. 

:  [Life  of]  ELIAS  LOOMIS.     New  Haven,  1890.     8vo.     P. 

:  Relation  of  Meteorites  to  Comets  (reprint  from  Nature ,, 

Vol  XIX).     n.  p.,  n.  d.     8vo.     P. 
:  To  describe  a  circle  tangent  to  three  given  circles  (from 

Math.  Monthly),     n.  p.,  n.  d.     Svo.     P. 
:  On  the   Geometrical  construction  of  certain  curves  by 

points.     (Cambridge),  n.  d.     Svo.     P. 

:  On  Shooting  Stars.     Washington,  n.  d.     4to.     P. 

and   TWINING    (A.    C.):  The   August   Meteors,  etc.     New 

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NEW    YORK    (American    Metrological    Society):    Proceedings. 

Vol.  II  (1878-9).     New  York,  1880.     Svo.     P. 
NEW  YORK  (Central  Park  Meteorological  Observatory) :  Annual 

Reports.     [Transferred  to  University  Library,  Berkeley.] 
NEW  YORK  (State  Library):  Catalogue  of  the  Books  on  Bibli- 
ography, etc.     Albany,  1858.     Svo. 
NEW  YORK  (State  Survey):  Reports  for  .the  years  1877-80-81- 

82-83-84.     6vols.     Albany.     Svo.     P.      ;*' 
NIAUDET    (A.):    Elementary    Treatise    on    electric    batteries. 

Translated  by  L.  M.  FISHBACK.     3d  edition.     New  York, 

1884.     Svo. 
NICE   (observatory):    Annales.      Vol.    II   (1887);  III    (1890). 

Text  and  Atlas.     Paris.     4to. 
NIESTEN    (L.):    Sur    1'aspect    physique    de    la    planete   Mars 

(1888).     Brussels,  1888.     Svo.     P. 
NIPHER  (F.  E.):  Choice  and  Chance;   a  lecture.     Kansas  City,. 

1880.     Svo.     P. 
:  Magnetic   Observations  in   Missouri,    1878.     n.  p.,  n.  d. 

Svo.     P. 
:  Magnetic  determinations  in  Missouri  in   1879.      n.  p.r 

n.  d.     Svo.     P. 


80*  Catalogue  of  the 


NIVEN  (W.  D.)  (editor):  See  MAXWELL. 

NOBILE   (A.):  Osservazioni  del  sistema  STRUVE  748.     Naples, 

1877.     4to.     P. 
:    Riflessioni  relative   alia  determinazione  telegrafica   di 

differenza  di  longitudine.     Naples,  1877.     4to.     P. 
:  Osservazioni  e  riflessioni  sui  sistemi  di  stelle  multiple. 

Naples,  1878.     4to.     P. 
:  Terza  determinazione  della  latitudine  del  R.  Osservatorio 

di  Capodimonte.     Naples,  1883.     folio.     P. 
:  SulP  impiego  di  uno  Stromento  meridiano  completo  nel 

primo  verticale.     (Naples),  1886.     4to.     P. 
:  Richerche  Numeriche  sulla  latitudine  del  R.  Osservatorio 

di   Capodimonte.     Parte    secunda,    1885.      Naples,    1888. 

folio.     P. 

:  II  cherchio   meridiano  del  R.  Osservatorio  di  Capodi- 
monte.    Naples,  1888.     4to.     P. 

:  Riflessioni  Geodetiche.     Naples,  1889.     folio.     P. 

NOLTHIUS  (A.):  Observatio  vnd  Beschreibung  des  Newen  Gome- 
ten/  so  vmb  das  ende  des  1572.     vnd  noch  in  diesem  73. 

Jar  erschienen/  Geschehen  vnd  gestellet/  Durch  ANDREAM 

NOLTHIUM    Mathematicum.     Gedruckt   zu   Erffurdt/  zum 

bundten  Lawen  bey  Sanct  Paul.     Erfurt,  1573.     4to. 
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a  comet.     New  Haven,  1859.     8vo.     P. 
:  COGGIA'S  Comet— its  physical  condition  and  structure. 

New  Haven,  1878.     8vo.     P. 
:  On  the    variability    of    the    ultimate    molecule.     New 

Haven,  1879.     8vo.     P. 
:  Theoretical  determination  of  the  dimensions  of  DONATI'S 

Comet.     (Continued.)     New  Haven,  n.  d.     8vo.     P. 
NOURSE  (J.  E.):  See  Washington  Observatory. 
NYREN    (M.):    De'clinaisons   moyennes    corrigees    des   etoiles 

principales   pour   Pepoque,    1845.0,   etc.    (1842-49).      St. 

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:  Untersuchung  der  REPSOLD'  schen  Theilung  des  Pulko- 

waer  Verticalkreises,  etc.     St.  Petersburg,  1886.     folio. 


Lick  Observatory  Library.  81* 

OAKLAND    (Cal.)     (Health     Department):      Monthly    Reports. 

[Transferred  to  University  Library,  Berkeley.] 
(The)  OBSERVATORY:  X  (1887);  XI  (1888);  XII  (1889),  XIII 

(current).     London.     8vo. 
OEHL  (E.):  Versuch  einer  Theorie  ueber  Kometen.     Vienna. 

8vo.     P. 
OELTZEN  (W.) :  Nachweisdes  Vorkommens  von  Sternen  aus  den 

ARGELANDER'   schen  Nordlichen   Zonen   in  anderen  Quel- 

len;   also,  Nachtrag;   also,  Zusammenstellung  v.  Quellen 

fiir  Sternoerter,  zwischen  -f  45°  und  -{-80°,  mit  Ausschluss 

der  ARGELANDER'  schen  Zonen.     3  papers,  bound  in  1  vol. 

Vienna,  1854,  et  seq.     8vo. 
:  Erganzungen  zur   Histoire   Celeste  und  einigen   andern 

Sternkatalogen.     1  vol.     Vienna,  1854.     8vo. 
:  Eigene   Bewegung    von   Fixsternen   abgeleitet   aus  der 

Vergleichung   der   Histoire    Celeste    mit   d.   ARGELANDER' 

schen  N.  Zonen.     1  vol.     Vienna,  1855.     8vo. 
:    SCHWERD'S     Beobachtungen    von     Circumpolarsternen. 

Vienna,  1855.     4to. 
:  ARGELANDER'S  Zonen-Beobachtungen  von  — 15°  bis  — 31° 

fur  1850.0.     Vienna,  1858.     8vo. 
• — : — •:  Vergleichungen  zwischen  den  Zonenbeobachtungen  von 

BESSEL  und  ARGELANDER.     Vienna.     8vo. 
OFFRET  (A.):  Sur  le  tremblement  de  terre  du  23  Fevrier,  1887. 

Paris,  n.  d.     4to.     P. 
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bound   in  1  vol.;    vols.    (6-7-8-9-10),   bound   in   1    vol. 

Halle,  1881.     4to. 
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[OHM  (G.  jS.)]:  See  LOMMEL. 
OLBERS    (W.):    Abhandlung    ueber    die    leichteste     *     *     * 

Methode  die  Bahn  eines  Cometen  zu  berechnen.     Heraus- 

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London,  1888.     12mo. 


82*  Catalogue  of  the 


OLMSTED  (D.):  Secular  Period  of  Aurora  Borealis.  Washing- 
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ONNEN  (H.):  See  FIGEE. 

OPPOLZER  (Th.):  Lehrbuch  zur  Bahnbestimmung  der  Kometen 
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8vo.  P. 

O'REILLY  (J.  P.):  1.  On  the  correlation  of  lines  of  direction 
on  the  Earth's  Surface  (1879).  2.  (On)  a  group  of  col- 
umnar basalts  (1879).  3.  Catalogue  of  earthquakes  in 
Great  Britain,  etc.  (1884).  4.  Catalogue  of  earthquakes 
in  Europe,  etc.  (1886).  (Bound  in  1  vor.)  Dublin.  4to. 

:  On  the  gaseous  products  of  the  Krakatoa  eruption,  etc. 

Dublin,  1885.  8vo.  P. 

:  On  the  antipodal  relation  of  the  New  Zealand  earthquake 

of  1886,  with  that  of  Andalucia,  1884.  Dublin,  1887. 
8vo.  P. 

OTTAWA  (Department  of  the  Interior):  Manual  of  Dominion 
Land  Surveys.  Ottawa,  1883.  12mo.  P. 

OTTE  (E.  C.):  £ee  HUMBOLDT. 

OUDEMANS  (J.  A.  C.):  Zweijaehrige  Beobachtungen  der  Veraen- 
derlichen  Sterne,  1855—56.  n.  p.,  n.  d.  4to. 

:  On  the  condition  that  in  a  double-image  micrometer  the 

value  of  a  revolution  *  *  *  be  independent  of  the 
accommodation  of  the  eye.  London,  n.  d.  8vo.  P. 

OXFORD  (Radcliffe  Observatory):  [First]  Catalogue  of  6317 
Stars  (JOHNSON).  Second  Catalogue  of  2386  Stars  (MAIN). 
2  vols.  Oxford,  1866  and  1870.  8vo. 

:  Results  of  Astronomical  Observations  in  1880-81-82-83- 

84-85.  Oxford.  8vo. 

OXFORD  (Savilian  Observatory) :  Reports,  14th,  1889.  n.  p.,  n.  d. 
8vo.  P. 


Lick  Observatory  Library.  83* 

OXFORD  (University  Observatory):   Astronomical  Observations. 

II  (UranometriaNova  Oxoniensis,  1885);  III  (Researches 

in    Stellar   Parallax   by   the  aid  of  Photography,   1889). 

Oxford,  1885-     8vo. 
PALERMO  (observatory):    Pubblicazioni.     Vol.  II  (1882-3);  III 

(1883-4-5);  IV  (1884-8).  -Palermo.     4to. 
PALISA  (J.):    Sternkarten.     No.  1.  22h  Om— 22h  20m;  —  9°— 14°; 

2.  10hOra— 10h21m;  +9°-f-14°;  3.  12h20m— 12h  41m;  —  0°30' 

-f  4°  45';  4.  9h  40m— 10h  Ora;   -fl5°+20°.     1878-85. 
PARIS  (Academy  of  Sciences):  Histoire  de  1'Academie  Royale 

des  Sciences,  avec  les  Memoires  de  Mathematique  et  de 

physique,  depuis  son  etablissement  en  1666  jusqu'en  1790 

[9  vols.  indexes].     119  volumes  in  4to.     Paris,  1699-1793. 
:    Machines   et    Inventions    approuvees   par    P Academic 

[1666-1754].     Vols.  1-7.     Paris,  1735-77.     4to. 
:  Memoires  donnes  a  1'Academie  Royale  des  Sciences  non 

imprimes   dans   leurs   temps — par   M.    FONTAINE.     Paris, 
.1744.     4to. 
:    Memoires  de  Mathematique  et   de  Physique   presentes 

*    *    *    par  divers  Savans.  Vols.  I,  II.  Paris,  1750-86.  4to. 
:  Recueil  des  pieces  qui  ont  remporte  les  prix,  etc.  [1720- 

72].     Paris,  1751-77.     4to. 
:  Nouvelles  Tables  des  Articles  contenus  dans  les  volumes 

de  1'Academie  Royal,  etc.,  1666-1770,  par  1'Abbe'  ROZIER. 

4  vols.     Paris,  1775.     4to. 
:  Tables  generales  des  travaux  contenus  dans  les  memoires 

de  1'Academie.     *     *     *     Premiere  serie,  tomes  I  a  XIV 

(an  VI,  1815).     Seconde  serie,  tomes  I  a  XL  (1816-78). 

Paris,  1881.     4to. 
See  BOUGUER. 

See  CASSINI.     See  CASSINI  DE  THURY. 
See  CHABERT. 
See  CONDAMINE. 
See  COURTANVAUX. 
[History  of.]     See  DUHAMEL. 

See  FONTENELLE. 

See  LACAILLE. 
See  MAIRAN.. 


84* 


Catalogue  of  the 


PARIS  (Academy  of  Sciences):  Table  generale  des  Comptes 
Rendus  des  seances  de  1'Academie  des  Sciences.  1  vol. 
Tomes  I-XXXI  (3  August,  1835,  to  30  December,  1850). 
1  vol.  Tomes  XXXII-LXI  (January,  1851,  to  30  Decem- 
ber, 1865).  1  vol.  Tomes  LXII-XCI  (January  2,  1866, 
to  December  27,  1880).  3.  vols.  Paris.  4to. 

PARIS  (Astronomical  Society  of  France):  Bulletin.  Premiere 
Annee,  1887;  Troisieme  Annee  (parts  3,  4,  5,  6,  7). 

PARIS  (Bureau  des  Longitudes):  Annales,  I  (1877),  II  (1882), 
III  (1883).  Paris.  4to. 

:  Annuaire,  1838;  185-,  -1-,  -3,  -4;  186-,  -,  -,  -,  -,  -5; 

_5  _}  _  _9 ;  1 870-1-2-3-4-5-6-7-8-9 ;  1 880-1 ,  -,  3-4-5-6-7- 
8-9.  Paris.  32mo. 

:  Connaissance  des  Temps,  1884,  -,6-7-8-9;  1890-1.  Paris, 

8vo. 

PARIS  (Congres  international  de  photographic  celeste) :  Proces- 
Verbaux  des  Seances.  Paris,  1889.  £vo.  P.  See  below. 

PARIS  (Conservatoire  des  Arts  et  Metiers):  Catalogue  des  Col- 
lections. Paris,  1882.  16mo. 

PARIS  (Department  of  Public  Instruction) :  Observatoires  astro- 
nomiques  de  province,  1881;  same,  1885;  same,  1887;  same, 
1888.  Paris.  8vo.  P. 

PARIS  (Ecole  Poly  technique) :  Journal  (Cashiers  47, 48,  49,  50)  ; 
(51,  52,  53,  54);  (55,  56,  57,  58).  3  vols.  Paris,  1880-89. 
4to. 

:  Catalogue  de  la  bibliotheque.     Paris,  1881.     8vo. 

PARIS  (International  Astro-Photographic  Congress):  Bulletins 
1,  2,  3,  4,  bound  in  1  vol.  Paris,  1887-9.  4to. 

PARIS  (National  Observatory):  Annales — Memoires,  6-7-8-9- 
10-11-12-13-14-15-16-17-18.  Paris,  1861-85.  4to. 

PARIS  (observatory):  Catalogue  de  1'Observatoire  de  Paris. 
Vol.  I  (Oh— 6h).  Paris,  1887.  4to. 

:  Ecliptic  Charts  by  CHACORNAC,  HENRY,  and  others.  1 

bound  volume,  containing: 


Nos. 

R. 

A. 

Dec. 

Nos. 

R 

A. 

Dec. 

8..  2* 

20' 

41m 

+12°  15'; 

-17°  307 

43-14h   0" 

1  21m 

—15°  45'  ; 

—10°  SO' 

10a    3 

0 

Q 

21 

+10      0; 

-15    15 

48..15  39 

—16 

2 

—22    45; 

—17    30 

10..  3 

0 

—  3 

21 

+15    15; 

-20    30 

59-19  19 

—19 

•42 

—24    30; 

—19    15 

33..10 

40 

—11 

1 

+  4    45; 

-10      0 

67-22     0 

—22 

21 

-14      0; 

—  8    45 

38-12 

20 

—12 

41 

-5    45; 

—  0    30 

68-22  20 

—22 

41 

—12     15; 

—  7      0 

39..12 

40 

—13 

1 

—  8      0; 

—  2    45 

69-22  40 

—23 

1 

—10      0; 

—  4    45 

Lick  Observatory  Library.  85* 

PARIS  (observatory):    Paper  prints  from  Stellar  photographs, 

by  MM.  HENRY.     1.  R.  A.  =  20h  4m  P  =  52°  15',  August  12, 

1885;  2.  R.  A,  =  19h  55m  P  =  52°  15',  August  13,  1885. 
PARTS    (National   Observatory):  Rapport   annuel,   1884,   1885, 

1886,  1887,  1888,  1889.     Paris.     4to.     P. 
PARIS  (Societe  d' Astronomic) :  See  Journal  du  Ciel. 
PARIS  (Universal  Exposition):  Reports  of  the  U.  S.  Commis- 

eioners,  Vols.  1-2-3-4-5-.     Washington,  1880.     Svo. 
PARIS  (Universal  Exposition,  1889):  Official  Catalogue  of  the 

U.  S.  Exhibit.     Paris,  n.  d.     Svo. 
PARIS  (University  of  Paris):  Le  livret  de  1'etudiant  de  Paris. 

Programmes  des  Cours,  1889-90.     Paris,  1889.     16mo. 
PAUL  (H.  M.):  A  determination  of  the  semi-diameter  of  the 

Moon  from  occultations,  etc.     Washington,  1883.    4to.    P. 
PEARSON  (W.):  An   introduction   to  Practical  Astronomy.     2 

vols.  text  and  1  vol.  plates.     London,  1824-9.     4to. 
PECHULE  (C.  F.):  Passage  de  Venus,  1882.     Copenhagen,  1883. 

Svo. 

PEEK  (C.  E.):  See  Rousdon. 
PEIRCE    (B.):    Address     *     *     on  retiring  from  the  duties  of" 

President  (A.  A.  A.  S.).     Salem,  1853.     Svo.     P. 

:  Tables  of  the  Moon.     Washington,  1865.     4to. 

[ ]:   (Biography  of.)     n.  p.,  n.  d.     Svo.     P. 

PEIRCE  (C.  S.):  *     *  •*     The  Logic  of  Relatives.     Cambridge, 

1870.     4to.     P. 
:    A   Quincuncial   Projection   of  the   Sphere.     Baltimore, 

1879.  4to.     P. 

:  On   the   ghosts    in    RUTHERFURD'S    Diffraction-Spectra. 

Baltimore,  1S79.     4to.     P. 
PEIRCE  (J.  M.):   Mathematical  Tables.     First  Series.     Boston, 

1880.  12mo. 

PENDLEBURY  (C.):  Lenses  and  systems  of  lenses.     Cambridge, 

1884.     Svo. 
PENROSE  (F.  C.):  A  method  of  Predicting  Occultations   and 

Solar  Eclipses.     London,  1869.     folio. 
PERRY  (S.  J.):  Observations  of  the  Total  Solar  Eclipse  of  Aug. 

29^  1886.     London,  1889.     4to.     P. 


86*  Catalogue  of  the 


PERRY. (S.  J.):  Phenomena  observed  upon  the  Solar  Surface, 

1881-84.     London,  n.  d.     8vo.     P. 
and  STEWART  (B.):     *      *      *      Comparison  of  certain 

simultaneous  fluctuations  of  [magnetic]   declination,  etc. 

London,  1885.     Svo.     P. 
PETERS  (C.  A.  F.):  Ueber  die  Bestimmung  des  Laengenunter- 

schiedes  zwischen  Altona  und  Schwerin.    Altona,  1861.  4to. 
:  Bestimmung  des  Laengenunterschiedes  zwischen  Altona 

und  Kiel.     Kiel,  1873.     4to. 
:  Bestimmung  des  Langenunterschiedes  zwischen  Gottin- 

gen  und  Altona.     Kiel,  1880.     4to.     P. 

PETERS  (C.  F.  W.) :  Astronomische  Tafeln  und  Formeln.    Ham- 
burg, 1871.     Svo. 
PETERS  (C.  H.  F.):  Memoria  sopra  la  nuova  Cometa  periodica 

di  IP.  anni.     Naples,  1847.     4to.     P. 
:  Longitude  of  Elmira.    Longitude  and  Latitude  of  Ogdens- 

burg.     Longitude  of  the  Western  Boundary  line   of  the 

State  of  New  York.     3  vols.     Albany,  1864-68.     Svo.     P. 
:  Celestial   Charts.     Nos.  1-20,   bound   in    1  vol.     Index 

accompanies  the  charts.     Washington,  1882.  _  folio. 
:  *     *     *     Catalogo   delle   Stelle    Contenate   nell'  Alma- 

.gesto  di  Tolomeo.     [Photographs  of  the  first  pages  of  8 

mss.  of  the  Almagest  accompany.]     Venice,  1884.     Svo. 
:    On   FLAMSTEED'S   Stars,   "observed  but  not   existing." 

Washington  (1885).     4to.     P. 
:  Corrigenda    in    various    Star-Catalogues.     Washington 

(1885).     4to.     P. 

:  Beitragzu  Veraenderlichen  Sternen.    Kiel,  1889.    4to.    P. 

PETERSON  (R.  E.):  Familiar  Science.    Philadelphia,  1856.    Svo. 
PETZVAL  (J.):    Integration    der  Differential  Gleichungen  von 

Linearen  Form.     Vienna,  1847.     4to.     P. 
:     Integration      der     Linearen      Differentialgleichungen. 

Vienna,  1853.     4to. 
PHILADELPHIA  (American  Philosophical  Society):  Proceedings 

for  1891  (current).     Philadelphia.     Svo.     P. 
PHILADELPHIA  (Franklin  Institute):  Journal.     Series  III,  Vols. 

96,  97.     Philadelphia.     Svo. 

PHILADELPHIA  (U.  S.  International  Exhibition):  Official  Cata- 
logue of  the  British  Section,  Part  I.     London,  1876.     4to. 


Lick  Observatory  Library.  87* 

PHILADELPHIA  (U.  S.  International  Exposition):  Report,  etc. 
Vols.  X,  XL  Washington,  1884.  8vo. 

PHILLIPS  (A.  W.):  See  BEEBE. 

PIAZZI  (G.):  Praecipuarum  Stellarum  Inerrantium  Positiones 
Mediae  ineunte  Seculo  XIX  ex  Observationibus  habitis  in 
Specula  Panormitana,  ab  anno  1792  ad  annum  1802.  Pa- 
lermo, 1803.  folio. 

:  Same  (1792  to  1813).     Palermo,  1814.     folio. 

PICKERING  (E.G.):  On  the  Endowment  of  Research.  Salem, 
1877.  8vo.  P. 

:  New  Planetary  Nebulae.     New  Haven,  1880.     8vo.     P. 

:  Light  of  Comparison  Stars  for  Vesta.  New  Haven,  1884. 

8vo.  P. 

:  Accurate  mountain  heights.     Boston,  1885.     8vo.     P. 

:  A  new  form  of  polarimeter.     Boston,  1885.     8vo.     P. 

:  A  photographic  study  of  the  Nebula  of  Orion.     Boston, 

1885.  8vo.     P. 

:  Early  experiments  in  telegraphing  sound.     Boston,  1885. 

8vo.     P. 
:  An  investigation  in   Stellar  Photography.     Cambridge, 

1886.  4to. 

— . — :  Atmospheric  Refraction.     Cambridge,  1886.     8vo.     P. 

:  Comparison  of  maps  of  the  ultra-violet  spectrum.     New 

Haven,  1886.     8vo.     P. 

:  On  the  Spectrum  of  2,  Ursas  Majoris.     New  Haven,  1890. 

8vo.     P. 

:  Observations  of  Variable  Stars  in  1884,  1885,  1886.     3 

numbers.     Boston.     8vo.     P. 

:  On  the  diffraction  produced  by  the  edges  of  the  Moon. 

n.  p.,  n.  d.     8vo.     P. 

:  See  LANGLEY. 

PICKERING  (W.  H.):  Photometric  Researches.  Cambridge, 
1880.  8vo.  P. 

:  Photography  of  the  infra-red  region  of  the  Solar  Spec- 
trum. Boston,  1884.  8vo.  P. 

:  Colored  media  for  the  photographic  dark-room.     Boston, 

1885.     8vo.     P. 

:  Methods  of  determining  the  speed  of  photographic  ex- 
posures.    Cambridge,  1885.     8vo.     P. 
14 


88*  Catalogue  of  the 


PICKERING  (W.  H.):  Total  Eclipse  of  the  Sun,  August  29, 1886. 

n.  p.,  n.  d.     4to.     P. 
PIHL   (0.  A.  L.):  Micrometric  examination  of  Stellar  Cluster 

in  Perseus.     Christiania,  1869.     4to.     P. 

:  On  Magnets.     Christiania,  1878.     8vo.     P. 

PLANA  (J.):  See  Turin. 

PLANTAMOUR  (E.):  Disquisitio  de  methodis  tradites  ad  Cometa- 

rum  Orbitas  determinandas.     Koenigsberg,  1839.     4to. 
,  WOLF  (R.),  and  HIRSCH  (A.):  Difference  de  Longitude — 

Righi-Kulm,  Zurich,  Neuchatel.     Geneva,  1871.     4to. 
and  HIRSCH  (A.):  Difference  de  longitude  entre  des  sta- 
tions Suisses.     Geneva,  1872.     4to. 
and  LOEW  (M.):  Difference  de  longitude  entre  Geneve  et 

Strasbourg  (1876).     Geneva,  1879.     4to. 
PLASSMAN  (J.):  Lichtwechsel  von  Alpha  Cassiopeise  im  Jahre, 

1889;  also,  Part  II  (1890).    Warendorf,  1889.    Ms.   4to.  P. 
POGGENDORFF  (J.  C.):  Biographisch-literarisches  Handworter- 

buch.     Vols.  1-2.     Leipzig,  1863.     8vo. 

:  Geschichte  der  Physik.     Leipzig,  1879.  _8vo. 

POGSON  (N.  R.):  Telegraphic  determination   of  the  difference 

of    longitude    between     *     *     *     and    the    observatory, 

Madras.     Madras,  1884.     4to. 

:  See  Madras  (observatory). 

POMPEII:  II  Rosario  e  la  nuova  Pompei;  periodico  mensuale. 

[Transferred   to   the  General  Library  of  the   University, 

Berkeley.] 

PONTECOULANT  (Ph.  G.  D.  de):  Memoire  sur  le  calcul  des  Per- 
turbations, et  de  la  Comete  de  HALLEY.    Paris,  1835.    4to. 
POOLE   (W.  F):  Index  to  Periodical  Literature.     3d  edition,  to 

1882.     Boston,  1882.     8vo. 
POORE   (B.  P.):  Catalogue  of  the  Government  Publications  of 

the  United  States,  1774-1881.     Washington,  1885.     4to. 
(The)  POPULAR  SCIENCE  NEWS:  Beginning  with  Vol.  24,  No.  6 

(June,  1890).     Boston.     4to.     P. 
PORRO  (F.):    Osservazioni   delle   Comete,  FINLAY  e  BARNARD- 

HARTWIG.     3  numbers.     Turin,  1887.     8vo.     P. 
:  Intorno  all'  Eclisse  totale  di  Luna  (January  28,  1888). 

Turin,  1889.     8vo.     P. 


Lick  Observatory  Library.  89* 

PORRO  (F.):  Sulla  differenza  di  longitudine  fra  gli  Osservatori 

di  Milano  e  di  Torino.     Turin,  1889.     8vo.     P. 
PORTER  (J.  G.):  Zone   catalogue   of  4050   Stars.     Cincinnati, 

1887.     4to. 
POTSDAM    (Astrophysikalische  observatorium):    Publicationen. 

Vols.  1,  2,  3,  4,  5,  6.     Leipzig,  1879-    4to. 
POWELL  (J.  W.):  On  the  organization  of  scientific  work  of  the 

[U.  S.].     Washington,  1885.     8vo.     P. 

:  See  Washington  (U.  S.  Geological  Survey). 

PRAGUE  (observatory):  Astronomische,  Magnetische  und  Meteor  o- 

logische     Beobachtungen      (1878-9,   1880-1-2-3-4-5-6-7), 

bound  in.l  vol.     Prague,     folio.     Also,  1888.     P. 
:    Astronomische  Beobachtungen     *     *     *     im  J.,  1884 

enthaltend   Originalzeichuungen    des   Mondes   von    Prof. 

L.  WEINEK.     Prague,  1886.     folio. 
PRESTON  (E.  D.):  Determinations  of  latitude  and  gravity  for 

the  Hawaiian  Government  [and  at  the  Lick  Observatory]. 

U.  S.  C.  &  G.  Survey,  Bulletin  No.  11.     Washington,  1889. 

4to.     P. 
:  Differential  method  of  computing  apparent  places,  etc. 

Philadelphia,  1889.     8vo.     P. 

PRICE  (J.  M.):  Interest  Tables.     New  York,  1856.     folio. 
PRIESTLEY  (J.):  The  History  and  Present  State  of  Electricity. 

Vol.  I.     London,  1775.     8vo. 
PRINCE  (C.  L.):  *     *     *     Account  given  by  HEVELIUS  of  the 

method  of  mounting  his  telescopes,  etc.     s.  L,  1882.     8vo. 
:    *     *     *     Climate   of  Crowborough  Hill,  Sussex,     s.  L, 

1885.     8vo. 
:  Observations  upon  the  climate  of  Uckfield,  Sussex,  etc., 

from  1843  to  1870.     3d  edition.     Lewes,  1886.     8vo. 
PRITCHARD    (C.):  Results   of  recent  investigations   of  Stellar 

parallax.     London,  1888.     8vo.     P. 

:  See  HERSCHEL.     See  Oxford. 

PRITCHETT  (H.  S.):  Ephemeris  of  the  Satellites  of  Mars  (1881). 

n.  p.,  n.  d.     8vo.     P. 

PROCTOR  (R.  A.) :  Sun  Views  of  Earth.     New  York,  1867.     4to. 
:  A  chart  of  the  Northern  Hemisphere     *     *     *     showing 

all  the  Stars  in  ARGELANDER'S  charts  (324198).     Manches- 
ter, 1871.     folio.     P. 


90*  Catalogue  of  the 


PROCTOR  (R.  A.):   The  Sun.     3d  edition.     London,  1876.     8vo. 
A  Star- Atlas  for  Students  and  Observers.     London,  1877. 


The  Universe  of  Stars.     2d  ed.     London,  1878.     8vo. 

Saturn  and  its  System.     2d  ed.     London,  1882.     8vo. 

A  Zone  of  Worlds  (from  N.  A.  Review).  New  York,  1884. 
8vo.  P. 

Half-hours  with  the  Stars.     London,  1884.     4to. 
Total   Solar   Eclipses    (from   the    Fortnightly   Review). 
London,  1886.     8vo.     P. 

Half-hours  with  the  Stars.     New  York,  n.  d.     4to. 
PTOLEMY:  Photographs  of  different  pages  of  mss.  of  the  Alma- 
gest, presented  by  Dr.  C.  H.  F.  PETERS.     Eleven  mounted 
photographs: 

Codex  Venet.  CCCII,  folio  8906;  CCC1II,  folio  142;  CCCX,  folio  90; 
CCCXI,  folio  201;  CCCXII,  folio  (?);  CCCXI1I,  folio  (?). 

Codex  Laurent.  Gr.,  I,  folio  102;  XLVII,  folio  1336;  XLVIII,  folio 
976.  Codex  Laurent.  Lat.,  XLV,  folio  (?);  Codex  Laurent.  Arab.,  CLVI, 
folio  776. 

:  See  HALMA.     See  PETERS  (C.  H.  F.). 

PULKOWA  (observatory):  Observations  de  Pulkova  publiees  par 

OTTO  STRUVE.     Vols.  1,  2,  3,  4, 5,  6, 7,  8,  9,  — ,  11, 12, 13, 14. 

St.  Petersburg,  1869.     4to. 
:    Catalogus  librorum  in  Bibliotheca  speculse  Pulcovensis. 

St«  Petersburg,  1860.     8vo. 
:  Catalogus  librorum,  etc.     Pars  secunda.     St.  Petersburg, 

1880.     8vo. 
:  Positions    moyennes   de    3542    etoiles   (extrait  du  Vol. 

VIII).     St.  Petersburg,  1886.     4to. 
:   Jahresbericht    fur    (1878-9   und   1879-80),   1881,    1882 

(1882-3  und  1883-4),  1885,  1886,  1887.     7  numbers.     St. 

Petersburg.     8vo.     P. 
QUARITCH  (B):  General  Catalogue  of  Books.     1  vol.     London, 

1868.     8vo. 

:  Same,  1871.     8vo. 

QUETELET  ( A.) :  Sur  la  difference  de  longitude  des  observatoires 

de  Bruxelles  et  de  Berlin  (1857).     Brussels,  n.  d.     4to. 
:  Sur  les  travaux  de  1'ancienne  Academie  de  Bruxelles. 

Brussels,  n.  d.     8vo.     P. 


Lick  Observatory  Library.  91* 

RAYET:  See  ANDRE. 

RAYMOND  (W.  G.):  What  constitutes  a  map?     San  Francisco. 

8vo.     P. 
REMSEN  (I.):  An  introduction  to  the  study  of  the  Compounds 

of  Carbon,  or  Organic  Chemistry.     Boston,  1887.     12mo. 
:  The  Principles  of  Theoretical   Chemistry.     3d   edition. 

Philadelphia,  1887.     8vo. 
RENAN  (H.):  See  LOEWY. 
RESPIGHI  (L.):    Declinazioni  medie   pel   1875.0   di  285  stelle 

[mags,  1-6;  from  +20°  to  +64°].     Rome,  1878.     4to. 
:  Catalogo   delle   declinazioni  medie   pel   1875.0  di  1463 

stelle  [+20°  to  +64°].     Rome,  1880.     4to. 
:  Catalogo   delle   declinazioni   medie  pel  1880.0  di  1004 

stelle  [from  0°  to  +20°,  and  from  4-64°  to  +90°].     Rome, 

1885.     4to. 
REULEAUX  (F.):  Der  Konstrukteur;  ein  Handbuch  zum  geb- 

rauch  beim  Maschinenentwerfen.     Parts  I,  II,  III,  bound 

in  1  vol.     Brunswick,  1882.     8vo. 
REYNAUD  (L.):  Memoir  upon  the  Illumination  and  Beaconage 

of  the   Coasts   of  France.     Translated   by   P.   C.  HAINS. 

Washington,  1876.     4to. 
RICE  (J.  M.)  and  JOHNSON  (W.  W.):  An  elementary  treatise 

on  the  Differential  Calculus.     New  York,  1885.     8vo. 
RICHARDSON  (W.):  See  BRISBANE. 
Rio  DE  JANEIRO  (National  Observatory):  Annales.     Vol.  II,  IV 

(i,  ii).     Rio,  1883,  et  seq.     4to. 
Rio  DE  JANEIRO  (observatory):   Anuario.    [Transferred  to  the 

Library  of  the  University  at  Berkeley.] 
RITCHIE  (J.):  The  Science  Observer  Code.     New  York,  1885. 

4to. 

:  See  CHANDLER. 

ROBERT  (H.  M.):  Rules  of  Order.     Chicago,  1885.     16mo. 
ROBERTS  (L):  Stellar  Photo-Engraving.     Liverpool.     8vo.     P. 
ROBINS  (E.  C.):  Technical  School  and  College  Building,  being 

a  treatise  on  the  design  and  construction  of  applied  science 

and  art  buildings,  and  their  suitable  fittings  and  sanita- 
tion, with  a  chapter   on   technical   education.      London, 

1887.     4to. 


92*  Catalogue  of  the 


ROBINSON  (H.  N.):  A  treatise  on  Astronomy.     New  York,  1859. 

8vo. 
ROCHE  (E.) :  Nouvelles  recherches  sur  la  figure  des  atmospheres 

des  corps  celestes.     Paris,  1862.     4to.     P. 
ROCHESTER  (Warner  Observatory):  History  and  Work  of  the 

WARNER  Observatory,  1883-86.     Vol.  I.     Rochester,  1887. 

8vo. 
ROCKWOOD  (C.  G.):  Japanese  Seismology.     New  Haven,  1884. 

8vo.     P. 

:  An  account  of  the   progress  of   vulcanology  and   seis- 
mology in  1886.     Washington,  1889.     8vo.     P. 
:  Notes  on  American  Earthquakes.    Nos.  11, 12,  13,  14,  15 

(1882-85).     5  numbers.     New  Haven.     8vo.     P. 
RODGERS  (J.):  On  the  usefulness  of  Government  Observatories. 

Washington,  1877.     8vo.     P. 
ROGERS  (H.  D.):  A  new  philosophy  of  the  Sun.     Buffalo,  1886. 

8vo.     P. 
ROGERS    (W.  A.):    On   the   present   state   of  the   question   of 

standards  of  length.     Boston,  1880.     8vo.  JP. 
:  Catalogue  of  1213   Stars,  observed  at  Harvard  College 

Observatory,  1870-79.     Cambridge,  1884.     4to. 
and  McLEOD  (C.  H.):  The  longitude  of  the  McGill  Col- 
lege Observatory.     Montreal,  1886.     4to.     P. 
:  On  a  practical   solution  of  the  perfect  screw  problem. 

n.  p.,  n.  d.     8vo.     P. 
ROME:  (R.  AccademiadeiLincei):  Rendiconti.   Vol.  Ill  (1887); 

IV,  Part  I  (1888);  IV,  Part  II  (1888);  V,  Part  I  (1889); 

V,  Part  II  (1889);  VI,  Part  I  (1890).     Rome.     4to. 
:   Transunti.     Vols.  V,  VI   (1881-2).     1  vol.     Vols.  VII, 

VIII  (1883-4).     1  vol.     Rome.     4to. 
ROME  (Italian  Spectroscopic  Society):  Memorie.     Vols.  1-2-3- 

4_5_6_7-8-9-10-ll-12-13-l  4-15-1 6-17.      [Presented     by 

E.  S.  HOLDEN.]     Rome,  1872.     4to. 
:  Memorie;  Appendice.     Vols.  Ill  (1874)  to  VIII  (1879), 

bound  in  1  vol.     Rome.     4to. 
[ROME  (observatory)]:  [Review  of  the]  Memoires  de  1'observa- 

toire,  1851-56.     Geneva,  n.  d.     8vo.     P. 


Lick  Observatory  Library.  93* 

ROSCOE  (H.  E.)  and  SCHORLEMMER  (C.):  A  treatise  on  Chemis- 
try.    Vols.  I,  II  (i,  ii),  III  (i,  ii).     New  York,  1884,  et  seq. 

8vo. 
ROSSE  (The  Earl  of):  On  the  construction  of  specula  of  six 

feet  aperture  and   a   selection   from   the  observations   of 

Nebulae  made  with  them.     London,  1862.     4to.     P. 
:  An  account  of  the  observations  on  the  Great  Nebula  of 

Orion.     *     *     *     between  1848  and  1867,  with  a  drawing 

of  the  nebula  [black  on  white  in  sections].     London,  1868. 

4to.     P. 
:  Note  on  the  Construction  of  Thermopiles.     London,  1870. 

8vo.     P. 
:  On  the  Radiation  of  Heat  from  the  Moon.     I  (1869),  II 

(1870).     2  numbers.     London.     8vo.     P. 
:  On  the  Radiation   of  Heat   from   the   Moon.     London, 

1873.     4to.     P. 
:  Notes    to    accompany     *     *    ,*     Drawings    of   Jupiter 

(1872-73).     London,    1874.     8vo.     P.     Also,  (Drawings). 
:  On  some  recent  improvements  made  in  the  mounting  of 

the  telescopes  at  Birr  Castle.     London,  1880.     4to.     P. 
:  Notes  on  the  Physical  Appearance  of  the  Comets  b  and  c, 

1881.     Dublin,  1882.     4to.     P. 
ROTCH  (A.   L.):  The   Blue   Hill   Meteorological   Observatory. 

Boston,  1887.     8vo.     P. 
ROUSDON    (observatory):   Astronomical   Observations,   1882-5. 

London,  1886.     4to.     P. 

:  See  Lyme-Regis. 

ROUTH  (E.  J.):  A  Treatise  on  the  Dynamics  of  a  System  of 

Rigid  Bodies.     2  parts.     2  vols.     London,  1882-84.     8vo. 
ROWLAND  (H.  A.):  Note  on  the  Theory  of  Electric  Absorption. 

Baltimore,  1878.     4to.     P. 
:    On   the   magnetic   effect   of  electric   convection.     New 

Haven,  1878.     8vo.     P. 
RUGBY   (Temple  Observatory):  Report  for  1880,  1886.     n.  p., 

n.  d.     8vo.     P. 
RUEMKER  (C.):  Preliminary  Catalogue  of  Fixed  Stars    *    *    * 

in  the  Southern  Hemisphere.     Hamburg,  1832.     4to. 
:  Mittlere  Oerter  von  12000  Fixsternen;  also,  Neue  Folge. 

Hamburg,  1843.     4to. 


94*  Catalogue  of  the 


RUNKLE  (J.  D.):  New  tables  for  determining  the  values  of  the 

Coefficients  in  the  Perturbative  Function,  etc.     (Asteroid 

supplement  to  the  above.)     Washington,  1855.     4to.     P. 
RUSH  (H.  G.):  The  true  doctrine  of  orbits.     Lancaster,  1887. 

8vo.     P. 
RUSSELL  (H.  C.):  Observations  on  the  Stars  and  Nebula  about 

Eta  Argus.     2  papers;  no  map.     Sydney,  1881.     8vo.     P. 
:  The   Coloured   Cluster,   about   Kappa    Crucis.     Sydney, 

1872.     8vo.     P. 
:    Local   particulars   of    the   Transit   of    Venus   in    1874. 

Sydney,  1873.     8vo.     P. 
:  Some  of  the  results  of  the  observation  of  the  Transit  of 

Venus  in  New  South  Wales.     Sydney,  1875.     8vo.     P. 

:  Climate  of  New  South  Wales.     Sydney,  1877.     8vo. 

:  Papers  read  before  the  Astronomical  Section  of  the  Royal 

Society,  N.  S.  W.,  1878.     Sydney,  1878.     8vo.     P. 
:  Some  results  of  an  astronomical  experiment  on  the  Blue 

Mountains.     Sydney,  1878.     8vo.     P. 
:  On  a  new  method  of  printing  Star  maps;  and  note  on 

conjunction  of  Mars  and  Saturn.     Sydney,  J.879.     8vo.     P. 

:  The  Gem  cluster  in  Argo.     Sydney,  1879.     8vo.     P. 

:  Recent  changes  in  the  surface  of  Jupiter.     Sydney,  1880. 

8vo.     P. 
:  The   Spectrum    and    appearance   of   the    recent   comet 

(1881).     Sydney,  1881.     8vo.     P. 

:  Transit  of  Mercury  (1881).     Sydney,  1881.     8vo.     P. 

:  Results   of    Double   Star   Measures,   1871-81.     Sydney, 

1882.     8vo. 
:  The  Sydney  Observatory;  History  and  Progress.   Sydney, 

1882.     8vo.     P. 

:  New  Double  Stars.     Sydney,  1883.     8vo.     P. 

:  Local  variations  and  vibrations  of  the  earth's  surface. 

Sydney,  1885.     8vo.     P. 
:  Astronomical  and  meteorological  workers  in  New  South 

Wales,  1778-1860.     Sydney,  1888.     Svo.     P. 
:  On  the  increasing  magnitude   of  Eta  Argus.     Sydney, 

1888.     Svo.     P. 
:  Proposed  method  of  recording  variations  in  the  direction 

of  the  vertical.     Sydney,  1888.     Svo.     P. 


Lick  Observatory  Library.  95* 

RUSSELL  (H.  C.):  Anniversary  Address  Royal  Society,  N.S.W., 

1877,1882,1885.     Sydney.     8vo.     P. 
:  President's  Address  at  the  first  meeting  of  the  Australian 

Assn.  Adv.  Sci.  (1888).     n.  p.,  n.  d.     8vo.     P. 

:  See  Sydney  (observatory). 

RUTHERFORD    (L.    M.):      Astronomical     Photography.       New 

Haven,  1865.     8vo.     P. 

:  Large  photograph  of  the  Moon,  October  4,  1873. 

SABINE  (E.):  See  St.  Helena. 

SACRAMENTO    (Dept.   of  Public   Instruction):    School   Law   of 

California.     Sacramento,  1885.     8vo. 

SACRAMENTO  (State  Library):  Catalogue,  1  vol.  (1866).     Cata- 
logue.    Vol.  I.     Law   Library   (1870).     Catalogue.     Vol. 

II.     General  Library  (1871).     Sacramento,  1866-71.     8vo. 
:  Catalogue  of   the    California    State    Library — General 

Department.     Sacramento,  1889.     8vo. 
SAFFORD  (T.  H.):  Catalogue  of  the  mean  declination  of  2018 

Stars.     Washington,  1879.     4to. 
:  Investigations   of  corrections   to   Greenwich   planetary 

observations,  1762-1830.     Washington,  1883.     4to.     P. 
:  Catalogue  of  North  Polar  Stars  (R.  A.).     Williamstown, 

1888.     4to.     P. 
:  The  development  of  Astronomy  in  the  United  States. 

Williamstown,  1888.     8vo.     P. 
ST.  HELENA  (Magnetic  Observatory):  Observations  by  General 

EDWARD  SABINE.     Vol.  II  (1844-49).     London,  1860.     4to. 
ST.  Louis  (Academy  of  Sciences):   Transactions.     Vols.  Ill  (No. 

4),  IV  (1,  2,  3),  V  (1,  2).     St.  Louis.     8vo.     P. 
ST.  PETERSBURG  (Academy  of  Sciences):    Melanges  mathema- 

tiques  et  astronomiques.      Vols.  I,  II,  III,  IV,  V,  VI  (1) 

(2  &  3).     St.  Petersburg,  1853.     8vo. 
ST.  PETERSBURG  (Central  Physical  Observatory):  Annalen  for 

1879-80-81-82-83.    Bound  in  1  vol.    St.  Petersburg.    4to. 
ST.  PETERSBURG   (University  Observatory):    Catalogus    libro- 

rum,  etc.     St.  Petersburg,  1888.     8vo.     P. 
SALEM  (American  Association  for  the  Advancement  of  Science) : 

Proceedings  (2-3-4)  (1849-50),  (6-7-8)  (1851-54),  (9-10) 

(1855-56),  (11-12  and  15)  (1857-58  and  1866),  29  (1881), 

34  (1885).     Salem.     8vo. 


96*  Catalogue  of  the 


SALEM  :  Report  (of  the  Philadelphia  meeting,  \  884,  from 
Science).  1  vol.  Cambridge,  1884.  8vo. 

:  Report  of  the  Committee  on  Standards  of  Stellar  Magni- 
tudes. -II-III-.  Salem.  8vo.  P. 

SALMON  (G.):  Treatise  on  conic  sections;  containing  an  account 
of  some  of  the  most  important  modern  algebraic  and  geo- 
metric methods.  6th  ed.  London,  1879.  8vo. 

:  Treatise  on  the  higher  plane  curves;  a  sequel  to  [the 

preceding].  3d  ed.  Dublin,  1879.  8vo. 

:  Treatise  on  the  analytic  geometry  of  three  dimensions. 

4th  ed.  Dublin,  1882.  8vo. 

:  Lessons  introductory  to  the  modern  higher  algebra.  4th 

ed.  Dublin,  1885.  8*vo. 

SAN  FERNANDO  (observatory):  Anales  del  Institute  y  Observa- 
torio  de  Marina.  Seccion  2a  Observaciones  Meteorologicas, 
1889.  [Transferred  to  the  Library  of  the  University  of 
California,  Berkeley.]  San  Fernando,  1890.  folio. 

SAN  FRANCISCO  (Astronomical  Society  of  the  Pacific):  Publica- 
tions. Vol.  I  (Nos.  1,  2,  3,  4,  5),  1889;  Vol.  II  (current). 
San  Francisco,  1889.  .  8vo. 

SAN  FRANCISCO:  Bulletin,  Examiner,  Chronicle  (are  presented  to 
the  Circulating  Library  of  the  L.  O.,  but  no  file  of  them  is 
kept). 

SAN  FRANCISCO  (California  Academy  of  Sciences):  Proceedings. 
2d  series.  Vol.  II  (1889).  San  Francisco.  8vo.  P. 

:  Bulletin.     I  (Nos.1-4),  (1884-6).     San  Francisco.     8vo. 

:  Constitution  and  By-Laws.     S.  F.,  1881.     32mo.     P. 

:  List  of  Honorary  and  Corresponding  Members.  1889.  Ms. 

SAN  FRANCISCO  (Free  Public  Library):  Catalogues,  1880-84, 
bound  in  1  vol.  San  Francisco,  n.  d.  8vo. 

SAN  JOSE  (University  of  the  Pacific):  The  Naranjado.  (San 
Jose),  1888.  8vo. 

SANTIAGO  (Hydrographic  office):  Anuario  Hidrografico  de  la 
Marina  de  Chile.  [Transferred  to  the  General  Library  of 
the  University  of  California  at  Berkeley.]  Santiago.  8vo. 

SANTIAGO  (observatory):  Meteorological  observations.  [Trans- 
ferred to  University  Library,  Berkeley.] 

SANTINI  (G.) :  Posizioni  medie  di  2706  Stelle  (—10°  e  —12°  30'). 
Venice,  1858.  4to. 


Lick  Observatory  Library.  97* 

SANTINI  (G.) :  Posizioni  medie  di  2246  Stelle  (—12°  30'  e  — 15°). 

Venice,  1862.     4to. 
SAWITSCH  (A):  Opposition  des  Mars  (1862).     St.  Petersburg, 

1863.     folio.     P. 
SCHAEBERLE  (J.  M.):  On  the  remarkable  Aurora  of  Sept.  12-13, 

1881.  New  Haven,  1881.     8vo.     P. 

:  A  method  for  determining  the  flexure  of  a  telescope,  etc. 

New  Haven,  1882.     8vo.     P. 
:  A  method  for  observing  artificial  transits.     New  Haven, 

1882.  8vo.     P. 

:  A  new  method  for  determining  the  Collimation  constant, 

etc.     New  Haven,  1883.     8vo.     P. 
:  Lateral    astronomical    refraction.      New    Haven,   1884. 

8vo.     P. 
:  A    short    demonstration    of  the    exponential    theorem. 

Univ.  of  Virginia,  1887.     8vo.     P. 
SCHAGEN  (P.):  Qvaestio  Naturalis  de  Terrae-Motv.     Cologne, 

1747.     4to. 
SCHEINER  (J.):  Vorlaufige  Mittheilung  ueber  Untersuchungen 

an    photographischen    Aufnahmen    von     Sternspectrum. 

Kiel,  1889.     4to.     P. 
SCHIAPARELLI    (G.    V.):    Osservazioni   astronomiche   e   fisiche 

*     *     *     sulla   topografia   del   pianeta   Marie.     I-II-III 

(1877,  1879-80,  1881-2),  bound  in  1  vol.     Rome,  1878-86. 

4to. 
:  Osservazioni  sulle  stelle  doppie  (1875-85).     Milan,  1888. 

folio. 
:  [Map  of  Mars  (1886),  transferred  to  a  globe  5  inches  in 

diameter,  by  J.  E.  KEELER.] 
SCHJELLERUP    (H.    C.    F.    C.):     Stjernefortegnelse,     *     *     * 

10000  Fixstjerner.     Copenhagen,  1864.     4to. 
:  Genaeherte  Oerter  der  Fixsternen  in  den  Astronomischen 

Nachrichten.     Band  1-66.     Leipzig,  1867.     4to. 
:  Description   des  Etoiles  Fixes     *     *     *     par  ABD-AL— 

RAHMAN  AL-Sun.     St.  Petersburg,  1874.     4to. 
SCHMIDT  (J.  F.  J.):  Ms.  drawing  of  Nebula  Orionis  on  a  scale 

of  2'=7mm.    [Presented  to  the  L.  0.  by  E.  S.  HOLDEN.] 

Athens,  1861. 
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98*  Catalogue  of  the 


SCHMIDT  ( J.  F.  J.) :  Charte  der  Gebirge  des  Mondes  nach  eigenen 
Beobachtungen, 1840-74.  1  portfolio  of  25  charts;  Erlaeu- 
terungsband.  1  vol.  4to.  Kurze  Erlaeuterung.  1  vol- 
4to.  P.  Berlin,  1878. 

SCHMITZ  (E.),  JULLIEN  (C.  E.),  and  LORENTZ  (E.):  Nouveau 
Manuel  Complet  de  1'Ingenieur  Civil.  Vols.  I,  II.  Paris, 
1845.  16nio. 

SCHMOLZ  (W.):  Weight  Tables  *  *  *  of  the  U.  S.  silver 
dollars.  San  Francisco,  1878.  8vo.  P. 

SCHOENFELD  (E.) :  Zweiter  Catalog  von  Verander  lichen  Sternen. 
Mannheim,  1875.  8vo.  P. 

:  Bonner  Sternkarten;  Zweite  Serie  (S.  D.).  1  copy  with 

maps  backed  with  linen  and  loose  in  portfolio.  1  copy 
with  maps  bound  in  1  vol.  Bonn,  1887.  folio. 

SCHORR  (H.) :  Untersuchungen  iiber  die  Bewegungsverhaltnisse 
in  dem  dreifachen  Sternsystem  £  Scorpii.  Munich,  1889. 
4to.  P. 

SCHOTT  (C.  A.):  Longitudes  determined  by  electric  telegraph 
between  1846  and  1885.  (U.  S.  C.  &  G.  Survey.)  Wash- 
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:  Magnetic  Dip  and  Intensity  in  the  U.  S.     Washington, 

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:  See  HAYES. 

:  See  KANE. 

:  See  MCCLINTOCK. 

SCHROETER  (J.  H.):  Areographische  Beitraege  (edited  by  H.  G. 
v.  d.  S.  BAKHUYSEN).  1  vol.  text;  1  vol.  atlas.  Leiden, 
1881.  8vo.,  etc. 

SCHULHOFF  (L.):  [On  Comet,  1873,  VII]  (in  Hungarian). 
Budapest,  1885.  8vo.  P. 

:  Recherches  sur  Porbite  de  la  Comete,  1873,  VII  (CoGQiA- 

WINNECKE).  Paris,  1886.  8vo.  P. 

:  Sur  les  orbites  des  Cometes,  1457  I  et  1818  I.     Paris, 

1887.  8vo.     P. 

and  BOSSERT   (J.):    Sur  1'orbite  de   la  Comete  de  1812. 

Paris,  n.  d.     4to.     P. 


Lick  Observatory  Library. 


SCHULTZ  (H.) :  Mikrometrische  Bestimmung  einiger  teleskopis- 

chen  Sternhaufen.     Stockholm,  1886.     8vo.     P. 
SCHULZ   (J.  F.  H.):    Zur  Sonnenphysik,  I,  II.     Vienna,  1888. 

8vo.     P. 
SCHUMACHER  (H.  C.):  Tafeln  zur  Reduction  der  in  der  Histoire 

Celeste   enthaltenen    Beobachtungen.     Copenhagen,    1825. 

16mo. 
:  Sammlung   von   Hiilfstafeln:    neu    herausgegeben    von 

G.  H.  L.  WARNSTOFF.     Altona,  1845.     8vo. 
SCHUMANN  (R.):  Ueber  den  gang  der  Pendeluhr  DENCKER  XII. 

Leipzig,  1888.     8vo.     P. 

SCHUMANN   (V.):    Die  brechbarsten  Lichtstrahlen,  ihre  photo- 

graphische  Energie,  etc.     n.  p.,  n.  d.     8vo.     P. 
SCHUR  ( W.) :  Untersuchungen  ueber  die  Bahn  des  Doppelsterns 

70  p  Ophinchi.     Altona,  1867.     4to.     P. 
— — :  Bestimmung   der  Masse  des   Planeten   Jupiter.     Halle, 

1882.     4to.     P. 
:  Ueber  die  Ausloeschung  des  Secundaeren  Spectrums,  etc. 

Berlin,  n.  d.     8vo.     P. 

SCHUSTER   (A.):    On    Spectra    of    Lightning.     London,   1879. 

8vo.     P. 
:  On  the   Spectra   of   metalloids:    Spectrum  of   oxygen. 

London,  1879.     4to.     P. 

:  See  LOCKYER. 

SCHWARZ  (L.):  See  Dorpat. 

SCHWEDOFF    (Th.):    Illusions    astronomiques.      Odessa,    1878. 

8vo.     P. 
:  Theorie  mathematique  des  formes  cometaires;  also,  Suite. 

Odessa,  1879.     8vo.     P. 
SCHWERD  (F.  M.):  Beobachtungen  von  circumpolar  Sternen  in 

Mitteren   positionen.     1828.0.      Von    WILHELM    OELTZEN. 

Vienna,  1855.     4to. 
SCHWOERER  (E.):  Relations  reciproques  des  grande  agents  de 

la  Nature,  etc.     Paris,  1886.     8vo.     P. 

:  Le  milieu  interstellaire,  etc.     Paris,  1889.     8vo.     P. 

SCIENCE:  Vols.  1,  2,  3,  4,  5,  6,  7,  8,  9, 11, 12, 13.    Cambridge  and 

New  York,  1883-89.     8vo. 


100*  Catalogue  of  the 


SCIENTIFIC  AMERICAN:  Vols.  59  (1888),  60  (1889),  61  (current). 

New  York.     4to. 
SEABROKE  (G.  M.):  Fourth  Catalogue   of  measures  of  double 

stars  at     *     *     *     Rugby.     London,  1885.     4to.     P. 
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of  sight.     London,  1887.     8vo.     P. 
SEARLE    (A.):    The  apparent  position  of  the   Zodiacal  light. 

Boston,  1885.     4to.     P. 
:  Atmospheric  economy  of  Solar  radiation.     Boston,  1888. 

8vo.     P. 
SECCHI  (A):  Le  Soleil.     2  vols  and  atlas.     Paris,  1875-7.     8vo. 

:  Ricerche  sulle  macchie  solari,  etc.     n.  p.,  n.  d.     4to.     P, 

:  Studi  fiscici  sulle  Comete  di  TEMPEL  II  e  COGGIA  III  nelr 

1874.     2a  Nota.     n.  p.,  n.  d.     folio.     P. 

SEE(T.  J.  J.):  Origin  of  Binary  Stars.    Columbia,  1889.  8vo.  P. 
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SEELIGER  (H.):  Untersuchungen  ueber  die  Bewegungsverhaelt- 

nisse   in  dem   Sternsystem    Zeta    Cancri.   JVienna,   1881. 

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:    Ueber  den  Einfluss  dioptrischer  Fehler  des  Auges  auf 

das  Resultat  astronomischer  Messungen.     Munich,  1886. 

4to.     P. 
SEIDEL   (L.):    Untersuchungen  iiber  die  gegenseitigen  Hellig- 

keiten  der  Fixsterne  erster  Grosse.     Berlin,  n.  d.     4to. 
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sternen.     Munich,  1867.     4to. 
Du  SEJOUR  (D.) :  Essai  sur  les  Phenomenes  relatifs  aux  dispari- 

tions  periodiques  de  Panneau  de  Saturne.     Paris,  1776.  8vo, 
SEKIYA   (S.):    Comparison  of  earthquake   diagrams     *     *     * 

obtained  by  two  instruments.     (Tokio),  n.  d.     4to.     P. 
SEYDLER  (A.):  Ueber  die  Bahn  des  ersten  Kometen  vom  Jahre 

1870.     Vienna,  1871.     8vo.     P. 

:  Ueber  die  Bahn  der  Dione.     Vienna,  1872.     8vo.     P. 

SHARPLESS  (I.) :  The  latitude  of  Haverford  College  Observatory, 

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SHDANOW  (A.):  Recherches  sur  1'orbite  intermediare  de  la  com- 

ete  de  FA  YE,  etc.     St.  Petersburg,  1885.     folio. 


Lick  Observatory  Library.  101* 

SIDEREAL    MESSENGER:    Vols.  1,  2,  3,  4,  5,  6,  7,  8.     Northfield, 

1882-89.     Svo. 
SILLIMAN   (B.)  An  account  of  the   meteor  which   burst   over 

Weston  in  December,  1807,  etc.     New  Haven,  1869.   Svo.  P. 

[ ]:  Life  of.    By  G.  P.  FISHER.    2  vols.    New  York,  1866.    Svo. 

SILLIMAN'S  JOURNAL:  See  American  Journal  of  Science. 
SIRIUS:  Zeitschrift  fur  populare  Astronomie.     Vol.  23  (or  new 

series,  vol.  17)  (1890).     Leipzig.     Svo. 
SMITH  (F.  H.)  and  STONE  (0.):  Transit  of  Venus,  1882.     Univ. 

of  Va.,  1883.     Svo.     P. 
SMITH  (N.  D.):  Meteorological  Observations  in  Arkansas  from 

1840    to    1859.      Washington,    Smithsonian    Institution, 

1860.     4to.     P. 
SMYTH  (C.  P.):    Carbon  and   Carbo-Hydrogen   spectroscoped, 

etc.,  in  1879.     London,  1879.     Svo.     P. 
:  The  Solar  Spectrum  in  1877  and  1878.     Edinburgh,  1879. 

4to.     P. 
:  Gaseous  Spectra  in  Vacuum  Tubes.     Edinburgh,  1881. 

4to.     P. 

:  On  the  constitution  of  the  lines  forming  the  low-tempera- 
ture Spectrum  of  Oxygen.     Edinburgh,  1882.     4to.     P. 
:  Micrometrical  Measures  of  Gaseous  Spectra  under  high 

dispersion.     Edinburgh,  1886.     4to. 
:  Mean  Scottish  Meteorology,  1856-87,  etc.     [Edinburgh], 

1888.     4to. 

:  Report  on  the  Royal  Observatory  (1888),  and  the  Edin- 
burgh Equatorial  in  1887,  etc.     [Reprint.]     n.  p.,  1888. 

Svo.     P. 

:  Madeira  Spectroscopic.     Edinburgh,  n.  d.     4to. 

SMYTH   (W.  H):   Cycle  of  Celestial  Objects;    2d  edition,  by 

G.  F.  CHAMBERS.     Oxford,  1881.     Svo. 
SOCOLOFF  (A.):  Sur  la  queue  du  I  type  de  la  Comete  de  1858y 

V.     Moscow,  1S84.     Svo.     P. 
SONNTAG  (A.):  Terrestrial  Magnetism  in  Mexico.     Washington,. 

Smithsonian  Institution,  1860.     4to.     P. 

SOUCHON  (A):  Traite  d' Astronomie  Pratique.    Paris,  1883.    Svo. 
SPECHT  (G.  J.):  Instructions  for  the  use  of  the  Improved  Slide 

Rule.     San  Francisco,  1879.     Svo.     P. 


102*  Catalogue  of  the 


SPENCER    (J.  W.):    Elevations   in   the   Dominion    of   Canada. 

Washington,  1884.     8vo.     P. 
SPIERS  and  SURENNE:  See  Dictionary. 

SPITALER  (R.):  Die  Astrophotographie.    Vienna,  1886.    8vo.    P. 
SPOERER   (G.):   Beobachtungen   der   Sonnenflecken.      Leipzig, 

1874.     4to. 
SPON  (E.)  and  others:  Workshop  Receipts.     Series  1,  2,  3,  4. 

London,  1888-9.     12mo. 
SPOOR  (J.  W.):  Electro- Astronomical  Atlas    [from   library  of 

JAMES  LICK].     Albany,  1874.     4to. 
STABIUS  (J.):  See  DURER. 
STEVENS  (W.  Le  C.):  Notes  on  Physiological  Optics.     London, 

1882.     8vo.     P. 

:  Physiological  Perspective.     London,  1882.  *  8vo.     P. 

:  The  Stereoscope.     I-II.     New  York,  1882.     8vo.     P. 

:  Sketch    of    Prof.   JOHN    LE    CONTE.     New   York,   1889. 

8vo.     P. 

:  The  Diffraction  of  Sound.     Philadelphia,  1889.    8vo.    P. 

STEWART  (B.)  and  GEE  (W.  H.  H.):  Lessons  i»  Elementary 

Practical  Physics.     2  vols.     London,  1885.     12mo. 

:  See  DE  LA  RUE. 

STOCKHOLM    (observatory):     Astronomiska    lakttalgelser   och 

Undersokningor.      Vol.   I,   Vol.   II    (1,  3).      Stockholm, 

1876-    4to. 
STOCKWELL  (J.  N.):  Secular  variations  of  the  Elements  of  the 

Orbits  of  the  Eight  Principal  Planets  [bound  with  other 

memoirs].     Washington,  1870.     4to. 
:  Theory   of    the    Moon's    motion.      Philadelphia,   1875. 

8vo.     P. 
:  On  the  inequalities  in  the  Moon's  motion,  produced  by 

the  oblateness  of  the  earth.     New  Haven,  1880.     8vo.     P. 
:  Recent   researches  in  the  lunar  theory.     New  Haven, 

1880.     8vo.     P. 
:  On  the  inequalities  in  the  Moon's  motion,  arising  from 

the  oblateness  of  the  earth.     Cambridge,  1886.     4to.     P. 
:  On  the  inequalities  of  long  period  in  the  Moon's  motion, 

arising   from    the    action    of    Venus.      Cambridge,   1887. 

4to.     P. 


Lick  Observatory  Library.  103* 

STOCKWELL  ( J.  N.) :  Secular  Variations  of  Orbits  of  the  Planets. 

Washington.     4to.     P. 
STONE  (E.  J.):  The  Cape  Catalogue  of  1159  Stars  for  1860.0. 

Capetown,  1860.     8vo. 
:  The   Cape   Catalogue   of   Stars   for   1840.0.     Capetown, 

1878.     8vo. 

:  Catalogue  of  12441  Stars  for  1880.     London,  1881.     4to. 

STONE  (0.):  On  the  determination  of  the  error  and  rate  of  a 

clock  by  the  method  of  least  squares,     n.  p.,  1881.     4to.    P. 

:  Nebula  of  Orion,  1885.     Univ.  of  Virginia,  1886.    8vo.    P. 

:  A  Quasi  Proof  of  the   Arithmetical  Mean.     n.  p.,  n.  d. 

8vo.     P. 

:  See  SMITH. 

STONYHURST  (observatory):  Results  of  Meteorological  and  Mag- 

netical  Observations  for  1882, 1883, 1884,  1885,  1886,  1.887, 

1888  (bound  in  1  vol.).     Roehampton.     16mo. 
STRING  HAM    (I.):    Regular    figures    in    n-dimensional    Space. 

Baltimore,  1880.     4to.     P. 
:  On  the  measure  of  inclination  of  two  planes,  in  space  of 

four  dimensions.     Berkeley  (1888).     Svo.     P. 
STROBL  (J.):  See  HERZ. 
STROUHAL  (V.):  See  BARUS. 
STRUVE  (H.):    FRESNEL'S  Interferenz-Erscheinungen.     Dorpat, 

1881.     Svo.     P. 
:  Ueber   die   allgemeine   Beugungsfigur    in   Fernroehren. 

St.  Petersburg,  1886.     folio.     P. 
:  Beobachtungen  der  Saturnstrabanten.    Erste  Abtheilung. 

St.  Petersburg,  1888.     folio.     P. 
STRUVE  (L.):  Resultate  aus  den  in  Pulkowa  angestellten  Ver- 

gleichungen  von  Procyon  mit  benachbarten  Sternen.     St. 

Petersburg,  1883.     folio.     P. 
:  Bestimmung   der   Constante   der   Praecession,  etc.     St. 

Petersburg,  1887.     folio.     P. 
STRUVE  (O.):  Beobachtung  der  totalen  Sonnenfinsterniss,  1851. 

St.  Petersburg,  1851.     Svo.     P. 
:  Nouvelle   determination  de   la  parallaxe  annuelle   des 

etoiles  Alpha  Lyras  et  61    Cygni.     St.   Petersburg,  1859. 

folio.     P. 
15 


104*  Catalogue  of  the 


STRUVE  (O.):  Beobachtung  der  totalen  Sonnenfinsterniss  vom 
18  Juli,  1860.  St.  Petersburg,  1861.  folio.  P. 

:  Uebersicht  der  Thatigkeit  der  Nicolai-Hauptsternwarte 

wahrend  der  ersten  25  Jahre  ihres  Bestehens.  St.  Peters- 
burg, 1865.  4to. 

:  Tabulse  Auxiliares  ad  transitus  per  planum  primum 

verticale  reducendos  inservientes.  St.  Petersburg,  1868. 
8vo. 

:  Mesures  micrometriques  Corrigees  des  Etoiles  Doubles. 

St.  Petersburg,  1879.  folio.  P. 

:  Etudes  sur  le  mouvement  relatif  des  deux  etoiles  du 

sy steme  de  61  Cygni.  St.  Petersburg,  1880.  folio.  P. 

:  Die  Beschliisse  der  Washingtoner  Meridian-Conferenz. 

St.  Petersburg,  1885.  8vo.  P. 

:  Sammlung  der  Beobachtungen  von  Sternbedeckungen 

waehrend  der  totalen  Mondfinsterniss,  1884,  October  4. 
St.  Petersburg,  1885.  8vo.  P. 

:  Die  Photographic  im  dienste  der  Astronomic.  St.  Peters- 
burg, 1886.  8vo.  P. 

:  Der  Nebelfleck  um  C  Orionis.  St.  Petersburg,  1887. 

8vo.  P. 

:  Tabula?  Quantitatum  Besselianarum  pro  annis  1750  ad 

1840Computatse.  Same,  1840-64.  Same,  1865-74.  Same, 
1875-79.  Same,  1885-89.  St.  Petersburg.  8vo. 

:  See  Pulkowa. 

— and  WINNECKE  (A.):  Pulkowaer  Beobachtungen  des 

Grossen  Cometen  von  1858.  St.  Petersburg,  1859.  folio. 

STRUVE  (W.):  Beschreibung  des  *  *  *.  grossen  Refractors 
von  FRAUENHOFER.  Dorpat,  1825.  folio. 

:  Stellarum  duplicium  mensuraB  micrometricse.  St.  Peters- 
burg, 1837.  folio. 

:  Description  de  1'observatoire  astronomique  central  de 

Poulkova.  1  vol.  text;  1  vol.  plates.  St.  Petersburg, 
1845.  4to. 

:  Sam.e.  Translated  into  English  for  the  use  of  the  Lick 

Trustees.  1  vol.  Ms.  folio. 

:  Etudes  d' Astronomic  Stellaire.  St.  Petersburg,  1847.  8vo. 

:  Ueber  den  HALLEY'  schen  Cometen  im  Jahre,  1835, 

Abtheilung  I.  Beobachtungen.  n.  p.,  n.  d.  folio. 

:  See  Dorpat. 


Lick  Observatory  Library.  105* 

SUFI:  See  SCHJELLERUP. 

SWIFT  (L.):  See  Rochester. 

SYDNEY  (observatory):  Astronomical  and  Meteorological  Ob- 
servations, 1859-60-61-62.  4vols.  Sydney ,1861-65.  8vo. 

:  Results  of  Astronomical  Observations,  1877-78.  Sydney, 

1881.  8vo. 

:  Results  of  Double  Star  Measures,  1871-81,  by  H.  C. 

RUSSELL.  Sydney,  1882.  8vo. 

:  Results  of  Meteorological  Observations.  Results  of  Rain 

and  River  Observations.  [Transferred  to  the  University 
Library,  Berkeley.] 

SYLVESTER  (J.  J.):  Address  to  the  Mathematical  Section,  B.  A. 
A.  S.,  1869.  London,  1869.  8vo.  P. 

SYRACUSE  (Central  Observatory):  Osservazioni  meteorologiche. 
[Transferred  to  the  University  Library,  Berkeley.] 

TACCHINI  (P.):  II  Passaggio  di  Venere  Sul  Sole  (1874).  Pa- 
lermo, 1875.  4to. 

:  Account  of  the  observations  of  the  Total  Eclipse  of 

April  6,  1875.  Rome,  n.  d.  folio.  P. 

:  See  HAGEN  and  HOLDEN. 

TACUBAYA  (National  Observatory):  Anuario,  1884-85-86, bound 
in  1  vol;  1887-88-89,  boundin  1  vol.;  1890.  Mexico.  16mo. 

(observatory):  Boletin,  Tomo  I  (1890).  Mexico,  1890.  4to. 

TAINTOR  (E.  C.):  Catalogue  of  384  Transit  Stars.  [Privately 
printed.]  Shanghai,  1878.  8vo.  P. 

TAIT  (P.  G.):  Heat.     London,  1884.     16mo. 

:  See  THOMSON. 

and  STEELE  (W.  G.):  A  Treatise  on  the  Dynamics  of  a 

Particle.     5th  edition.     London,  1882.     8vo. 
TASCHKENT  (observatory):  Annales  (in  Russian).     Vols.  I,  II, 

bound  in  1  vol.     Vol.  III.     P.     Moscow,  1885-9.     4to. 
TAUCHNITZ  (K.):  See  Dictionary. 
TAYLOR  (W.  B.):  Kinetic  theories  of  gravitation.     Washington, 

1877.     8vo.     P. 

:  A  memoir  of  JOSEPH  HENRY.    Washington,  1880.    8vo.    P. 

:  Physics     and    occult     qualities.       Washington,     1882. 

8vo.     P. 
:  On  the  crumpling  of  the  Earth's  Crust.     New  Haven, 

1885.     8vo.     P. 


106*  Catalogue  of  the 


TEBBUTT    (J.):    History   and   Description    of   Mr.   TEBBUTT'S 

Observatory,  Windsor,  N.  S.  W.     Sydney,  1887.     8vo.     P. 
:  Results   of  observations   of  comets  VI  and  VII,  1886. 

Sydney,  1887.     8vo.     P. 

:  Observations  of  Comet  a,  1888.    London,  1888.    8vo.    P. 

:  Results     of    observations    of    comets   I   and    II,  1888. 

Sydney,  1888.     8vo.     P. 
:  Report  of  Mr.  TEBBUTT'S  Observatory  for  1888.     Sydney. 

8vo.     P. 
(The)    TECHNOLOGY    QUARTERLY:    Vol.   Ill    (1890).      Boston, 

1890.     8vo.     P. 

TEJERA  (M.):  Origen  del  Mundo.     Barcelona,  1889.     8vo.  < 
TEMPELHOFF:  See  Berlin. 

TENNANT  (J.  F.):  Report  on  the  Transit  of  Venus,  1874.     Cal- 
cutta, 1877.     4to. 
TERBY  (F.):  1.  Areographische  Fragmente  (SCHROETER),  1873. 

2.  Are'ographie    (1636-1873).      3.  Ensemble  des  observa- 
tions physiques  de  la  planete  Mars  (1889).     Bound  in  1 

vol.     Brussels,  1873-89.     4to. 
:  Aspect   de   la   planete  Jupiter  (1872).     Brussels,  1872. 

8vo.     P. 
:  Configurations  des  taches  de  la  planete  Mars     *     *     * 

d'apres  les  dessins  inedits  de  SCHROETER.     Brussels,  1873. 

8vo.     P. 
:  Note  sur  une  configuration  singuliere  des  taches  de  la 

planete  Mars  (1862),  etc.     Brussels,  1873.     8vo.     P. 
:  Observations  de  Jupiter  et  de  Mars  (1873).     Brussels, 

1873.     8vo.     P, 
:  Remarques  sur  1'aspect  de  la  planete  Jupiter  (1874),  etc. 

Brussels,  1874.     8vo.     P. 
:  Sur  1'aspect  de  Pombre  du  2  ieme  Satellite  de  Jupiter 

[1874,  March  25].     Brussels,  1875.     8vo.     P. 
:  Un  dernier  mot  en  reponse  a  M.  FLAMMARION.     Brussels, 

1877.     8vo.     P. 
:  Etudes  sur  la  planete  Mars  (11  Notice).     Brussels,  1878. 

Svo.     P. 
:  Aspect  de  la  planete  Mars,  etc.  (1879).     Brussels,  1880. 

Svo.     P. 
:  Memoire  a  1'appui  des  observations  de  M.  SCHIAPARELLI 

sur  la  planete  Mars.     Brussels,  1880.     Svo.     P. 


Lick  Observatory  Library.  107* 

TERBY  (F.) :  Observations  des  Cometes  b  et  c  de  1881.  Brussels, 
1881.  8vo.  P. 

:  Aspect  de  la  grande  Comete  de  1882.  Brussels,  1882. 

8vo.  P. 

:  Aspect  et  position  de  la  grande  Comete  de  1882.  Brus- 
sels, 1883.  8vo.  P. 

:  Observation  de  la  lumiere  Zodiacale,  etc.  (1883).  Brus- 
sels, 1883.  8vo.  P. 

:  Observations  des  etoiles  filantes  periodiques  (1882). 

Brussels,  1883.  8vo.  P. 

:  Phenomenes  des  Satellites  de  Jupiter  (Oct.  14,  1883), 

etc.  Brussels,  1883.  8vo.  P. 

:  Note  sur  la  Comete  de  1812.     Brussels,  1884.     8vo.     P. 

:  Note  relative  a  la  gemination  des  Canaux  de  Mars. 

Brussels,  1885.  8vo.  P. 

:  Note  sur  la  pluie  d'etoiles  filantes  (Nov.,  1885).  Brus- 
sels, 1885.  8vo.  P. 

:  Etudes  sur  Paspect  physique  de  la  planete  Jupiter. 

Part  I  (1881-2).  Part  II  (1882-5).  Bound  in  1  vol. 
Brussels,  1885-7.  4to. 

:  Phenomenes  observes  sur  Saturne.  Brussels,  1887. 

8vo.  P. 

:  Sur  une  observation  de  Saturne.    Brussels,  1887.    8vo.    P. 

:  Etudes  sur  la  planete  Mars.  Notice  8-9-10-11-12. 

Brussels.  8vo.  P. 

:  Remarques  a  propos  des  observations  de  M.  SCHIAPARELLI 

sur  la  planete  Mars.  London,  n.  d.  8vo.  P. 

THAYER  (R.):  Earthquakes.     Philadelphia,  1886.     8vo.     P. 

THIELE  (T.  N.):  Castor.     Kopenhagen,  1879.     8vo.     P. 

:  Om  anvendelse  af  mindste  Kvadraters  Methode  i  nogle 

Tilfaelde,  etc.  Copenhagen,  1880.  4to.  P. 

THIEME-PREUSSER:  See  Dictionary. 

THOMPSON  (J.):  A  History  and  Handbook  of  Photography. 
(Translated  from  the  French  of  G.  TISSANDIER.)  New 
York,  1876.  8vo. 

THOMPSON  (S.  P.):  Elementary  Lessons  in  Electricity  and 
Magnetism.  London,  1887.  16mo. 

THOMPSON  &  WEST:  Historical  Atlas  Map  of  Santa  Clara 
County,  California.  San  Francisco,  1876.  folio. 


108*  Catalogiie  of  the 


THOMSON  (J.  J.):  A  treatise  on  the  motion  of  Vortex  Rings. 
London,  1883.  8vo. 

THOMSON  (W.)  and  TAIT  (P.  G.):  Handbuch  der  Theoretischen 
Physik.  Vol.  I,  Parts  i,  ii  (1  vol.).  Brunswick,  1871-74. 
8vo.  [Loaned  to  the  L.  O.  by  GEORGE  F.  BECKER,  Ph.D.] 

:  Elements  of  Natural  Philosophy.  Part  I,  2d  edition. 

Cambridge,  1879.  8vo. 

TIFLTS  (observatory):  Meteorological  Observations,  1880-86. 
1  vol.  Tiflis.  8vo. 

:  Magnetic  Observations.     Tiflis,  1879-87.     8vo. 

:  Beobachtungen  der  temperatur  des  Erdbodens  im  Jahre, 

1880,  1881,  1882,  1883.  Tiflis,  1881-85.  4to. 

TIFLIS  (Physical  Observatory):  Magnetische  Beobachtungen. 
Meteorologische  Beobachtungen.  [Transferred  to  the  Uni- 
versity Library,  Berkeley.] 

TISCHNER  (A.):  Sta,  Sol,  Ne  Moveare.     Leipzig.     8vo. 

TISSERAND  (F.):  Memoire  sur  les  deplacements  seculaires  du 
plan  de  1'orbite  (de  Japhet).  Toulouse,  n.  d.  8vo.  P. 

:  Traite  de  Mecanique  Celeste.    I,  II.    Paris,jL  889-91.    4to. 

TITTMAN  (0.  H.):  On  the  relation  of  the  yard  to  the  meter. 
Bulletin,  U.  S.  C.  &  G.  Survey,  No.  9.  Washington,  1889. 
4to.  P. 

TODD  (D.  P.):  Continuation  of  DAMOISEAU'S  Tables  of  the  Sat- 
ellites of  Jupiter  to  1900.  Washington,  1876.  4to. 

:  Observations  of  the   transit  of  Mercury,'  1878.     Salem, 

1879.  8vo.     P. 

:  On  an  attachment  for  equatorial  mountings,  etc.     Boston, 

1880.  8vo.     P. 

:  *     *     *     Search   for   a  trans-Neptunian   planet.     New 

Haven,  1880.     8vo.     P. 
:  On  the  use  of  the  electric  telegraph  during  Solar  eclipses. 

Boston,  1881.     8vo.     P. 
:  An  account  of  observations  of  the  transit  of  Venus,  1882, 

made  at  the  Lick  Observatory.    New  Haven,  1883.    8vo.    P. 
:  The  Lick  Observatory  (from  Science).     New  York,  1885. 

16mo.     P. 
:  Instructions  for  observing  the  Total  Eclipse  of  the  Sun, 

January  1,  1889.     Amherst,  1888.     4to.     P. 


Lick  Observatory  Library.  109* 

TODD  (D.  P.):  Preliminary    Report   (unofficial)    on  the   Total 

Solar  Eclipse  of  1887.     Amherst,  1888.     8vo.     P. 
:  American  Telescopes,     n.  p.,  n.  d.     8vo.     P. 

TODHUNTER  (I.):    A  History   of    the    Theory   of   Probability. 

Cambridge,  1865.     8vo. 
:  An  elementary  Treatise  on  LAPLACE'S  functions,  LAME'S 

functions,  and  BESSEL'S  functions.     London,  1875.     8vo. 
:  Mechanics   for   beginners,  with  key.     2  vols.     London, 

1882  and  1885.     32mo. 
:  An   elementary  treatise   on   the   Theory  of  Equations. 

London,  1885.     8vo. 

TOKIO  (observatory):  Annales.  Vol.  I,  Parts  i,  ii.  Tokio, 
1889.  4to. 

TOKIO  (Seismological  Society  of  Japan):  Transactions  (4-5), 
1882;  bound  in  1  vol.  (10-11-12)  (1887-8),  bound  in  1 
vol.;  13  (ii),  14,  Tokyo.  8vo. 

TOULOUSE  (observatory).     See  DARQUIER. 

TRIESTE  (observatory):  Astronomisch-nautische  Ephemeriden 
fur  das  Jahr,  1890.  Trieste,  1888.  8vo. 

TROUVELOT  (L.):  On   the  veiled   Solar   Spots.     Boston,  1875. 

8vo.     P. 
:  Spectres  fugitifs  observes  pres  du  limbe  solaire.     Paris, 

1880.     8vo.     P. 

:  Observations  on  Jupiter.     Boston,  1881.     8vo.     P. 

:  Astronomical  Drawings;  Manual.    New  York,  1882.    8vo. 

[The  drawings  are  framed,  and  hung  in  the  observatory.] 
:  Pastel  drawing  of  Saturn  (1874),  (large  size).   [Presented 

to  the  L.  O.  by  E.  S.  HOLDEN.] 

TROWBRIDGE  (D.):  On  the  nebular  hypothesis.  New  Haven, 
1864.  8vo.  P. 

TROWBRIDGE  (J.):  Methods  of  measuring  electric  currents  of 
great  strength,  etc.  Boston,  1878.  8vo.  P. 

and  SABINE  (W.  C.):  Wave  lengths  of  metallic  spectra  in 

the  ultra  violet.  Boston,  1888.  8vo.  P. 

TURIN  (Associazione  Italiana  per  le  osservazioni  delle  meteore 
luminose).  Osservazioni.  Anno  XIX  (1888).  Turin. 
16mo.  P. 


110*  Catalogue  of  the 


TURIN  (observatory):    Observations   Astronomiques   faites   en 

1822-1823-1824-1825,  a  1'observatoire  Royal  de  Turin,  par 

J.  PLANA.     Turin,  1828.     4to. 
:  Bolletino;    Osservazioni    meteorologiche;    Ejfemeridi,    etc. 

[Transferred  to  the  General  Library  of  the    University, 

Berkeley.] 
TURNER  (H.  H.):  Observations  of  the  Total  Solar  Eclipse  of 

Aug.  29,  1889.     London,  1884.     4to.     P. 
:  Results  obtained  with  the  personal  equation  machine  at 

Greenwich.     London,  n.  d.     8vo.     P. 
TWINING  (A.  C.):  The  doctrine  of  parallels,  etc.     New  Haven, 

1872.     8vo.     P. 

[TYCHO  BRAKE]  :  Life  of.     See  DREYER. 
TYNDALL  (J.):  On  Radiation.     New  York,  1865.     16mo. 
[ ]:  Proceedings   at   the    Farewell    Banquet   to   Professor 

TYNDALL.     New  York,  1873.     12mo.     P. 
UBAGHS    (P.):    Notice   sur   1'observatoire   de   Cointe    (Liege). 

Brussels,  1886.     8vo.     P. 

UNITED  STATES  OF  AMERICA:  Catalogue  of  Government  publica- 
tions to  1885.     See  POORE. 

UNIVERSITY  OF  VIRGINIA  (McCoRMicK  Observatory):    Publica- 
tions.    Vol.  I,  Part  II  (Comet  1882,  II).     Univ.  of  Va., 

1886.     8vo.     P. 
UNIVERSITY  OF  VIRGINIA  (observatory):  Reports  for  1886, 1887, 

1888.     n.  p.     P. 
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Lick  Observatory  Library.  ill* 

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WASHINGTON  (American  Ephemeris):  For  the  years  1856-7-8-9, 
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WASHINGTON  (Philosophical  Society):  Bulletin.  (1-2-3-4-5) 
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WASHINGTON  (Smithsonian  Institution):  Contributions  to 
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WASHINGTON  (U.  S.  Bureau  of  Ethnology):  Annual  Reports.  I 
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WASHINGTON  (U.  S.  Census  Bureau):  Ninth  census  of  the 
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WASHINGTON  (U.  S.  Coast  and  Geodetic  Survey):  Reports. 
1851*-2-3-4-5-6-7-8-9;  1860-1-2-3-4-5-6-7-8-9;  1870- 
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WASHINGTON  (U.  S.  Coast  Survey):  Coast  Pilot  of  California, 
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WASHINGTON  (U.  S.  Engineer  Department):  Report  on  the 
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primary  stations  at  Cheyenne,  Wyoming  Territory,  and 
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*  With  volume  of  sketches,     f  Index.    %  Index  to  charts. 


114*  Catalogue  of  the 


WASHINGTON  (U.  S.  Geographical  and  Geological  Survey): 
Report  on  the  lands  of  the  arid  region  of  the  United 
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WASHINGTON  (U.  S.  Geological  Survey):  Annual  Reports  (by 
C.  KING  and  J.  W.  POWELL).  I  (1879-80),  II,  III,  IV,  V, 
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:  Mineral  Resources  of  the  United  States.  Calendar  year, 

1887.  Washington,  1888.  8vo. 

WASHINGTON  (U.  S.  Hydrographic  office):  Catalogue  of  charts, 
etc.  Washington,  1887.  8vo.  P. 

WASHINGTON  (U.  S.  Lighthouse  Board):  Instructions  to  Light 
Keepers.  Washington,  1881.  4to. 

:  *  *  *  Effects  of  the  Earthquakes  of  1886  upon  cer- 
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:  Annual  Report  for  the  year  ending  June  30;  1874,  1875, 

1876,  1877, 1878,  1879,  1880,  1881,  1882,  1883,  1884,  1885, 
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WASHINGTON  (U.  S.  Medical  Department):  A  Report  on  the 
Hygiene  of  the  U.  S.  Army.  Washington,  1875.  4to. 

WASHINGTON  (U.  S.  Naval  Observatory):  Astronomical  [and 
Meteorological]  Observations  made  at  the  National  [U.  S. 
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Reports  on  Observations  of  the  Total  Eclipse  of  the  Sun, 

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Founding   and   Progress   of    the  Observatory,  by  J.  E. 

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Reports  on  the  removal  of  the  U.  S.  Naval  Observatory. 

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Reports  on  Observations  of  the  Transit  of  Mercury,  1878. 

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Reports  on  the  Total  Solar  Eclipses  of  July  29,  1878, 

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:  Zones  *  *  *  observed  with  the  Transit,  1846-49. 

1870.  4to. 

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WASHINGTON  (U.  S.  Northern  Boundary  Commission):  Decima- 
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1861.  4to. 

WASHINGTON  (United  States  Scientific  Expedition  to  West 
Africa,  1889.  D.  P.  TODD,  Director):  Bulletins.  Nos.  2,  4, 
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WASHINGTON  (U.  S.  Signal  Office):  Instructions  to  Observers. 
Washington,  1881.  8vo.  P. 

:  Signal  Service  Notes  (Nos.  6  to  23),  bound  in  1  vol. 

Washington,  1883-5.  8vo. 

:  Signal  Service  Papers  (8vo),  1872-86,  bound  in  1  vol. 

Washington.  8vo. 

:  Bulletin  of  International  Meteorology,  September,  1880, 

to  December,  1882.  Washington.  4to. 

:  Daily  Bulletin  of  Weather  Reports  for  the  year  1873. 

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WASHINGTON  (U.  S.  Transit  of  Venus  Commission):  Papers 
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116*  Catalogue  of  the 


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WASHINGTON  (U.  S.  Treasury  Department):  Letter  from  the 
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1836,  by  issues  and  redemptions,  and  from  January  1, 
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WASHINGTON  (U.  S.  War  Department):  Reports  of  the  explora- 
tions and  surveys,  to  ascertain  the  most  practicable  and 
economical  route  for  a  railroad  from  the  Mississippi  River 
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WATSON  (H.  W.):  The  Elements  of  Plane  and  Solid  Geometry. 
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WEBB  (J.  B.):  The  Second  Law  of  Thermodynamics.  Salem, 
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WEINEK  (L.):  Zeichnungen  von  Mars  und  dem  Zodiakallicht. 
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118*  Catalogue  of  the 


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Lick  Observatory  Library.  119* 

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:  On  the  form  and  position  of  the  sea  level.     Washington, 

1888.     8vo.     P. 

:  Formulas  and  Tables  to  facilitate  the  construction  of 

maps.     Washington,  1889.     8vo.     P. 

:  Latitudes  and  longitudes    *     *     *   in  Missouri,  Kansas, 

and  New  Mexico.     Washington,  1889.     8vo.     P. 

and  others:  *     *     *     Variations  in  length  of  certain  bars 

at  the   temperature   of  melting  ice.     New  Haven,  1883. 
8vo.     P. 

WORCESTER  (J.  E.):  See  Dictionary. 
WORTHEN  (W.  E.):  See  Encyclopaedia. 

YARNALL  (M.):  Catalogue  of  stars  observed  at  the  U.  S.  Naval 
Observatory.     2d  edition;  3d  edition  (edited  by  E.  FRISBY). 
Washington,  1873-89.     4to. 
YOUMANS  (E.  L.):  The  Correlation  and  Conservation  of  Forces. 

New  York,  1865.     8vo. 
YOUNG  (C.  A.):  Note  on  the  Spectrum  of  the  Corona.     New 

Haven,  1871.     8vo.     P. 

:  Preliminary  Catalogue  of  the  Bright  lines  in  the  Spec- 
trum of  the  Chromosphere.     New  Haven,  1871.     8vo.     P. 

:  Catalogue  of  Bright  lines  in  the  Spectrum  of  the  Solar 

Atmosphere,  observed   at   Sherman,   1872.     New   Haven, 
1872.     8vo.     P. 

Note  on  recurrent  vision.     New  Haven,  1872.     8vo.     P. 
Observations  of    ENCKE'S  Comet  [1871].     New  Haven, 
1872.     8vo.     P. 

The  Sun.     New  Haven,  1872.     16mo.     P. 
Note  on  the  use  of  a  diffraction  grating  as  a  substitute 
:br  prisms,  etc.     New  Haven,  1873.     8vo.     P. 
The  Constitution  of  the  Sun.     New  York,  1874.     8vo.     P. 
American  Astronomy;  its  history,  present  state,  needs, 
and  prospects.     Salem,  1876.     8vo.     P. 

Displacement  of  lines  in  the  Solar  Spectrum,  caused  by 
the  Sun's  rotation.     New  Haven,  1876.     8vo.     P. 

Note  on  the  Duplicity  of  the  1474  line  in  the  Solar  Spec- 
trum.    New  Haven,  1876.     8vo.     P. 
16 


120*  Catalogue  of  the 


YOUNG  (C.  A.):  Observations  upon  the  Solar  Eclipse  of  July 

29,  1878.     New  Haven,  1878.     8vo.     P. 
:  Results   of  the  Recent   Eclipse  [July  29,  1878].     New 

Haven,  1878.     8vo.     P. 
:  A   method   of   investigating   the   errors      *      *      *     of 

pivots.     Salem,  1879.     8vo.     P. 
:  Note  on  the  Spectrum  of  BRORSEN'S  Comet.     New  Haven, 

1879.     8vo.     P. 
:  Measures  of  the  diameters  of  Mars.     New  Haven,  1880. 

8vo.     P. 
:  Recent   progress   in   Solar   Astronomy   (from  Princeton 

Review,  January,  1880).     n.  p.,  1880.     8vo.     P. 
:  The  Color  Correction  of    *     *     *     object  glasses.     New 

Haven,  1880.     8vo.     P. 
:  Spectroscopic   observations    upon    the   Comet   6,   1881. 

New  Haven,  1881.     8vo.     P. 
:  The  Geographical  position  of    *     *     *     Princeton,  N.  J. 

London,  1881.     8vo.     P. 
:  The  23-inch  telescope  of  the  Halsted  Observatory.  Salem, 

1882.  8vo.     P. 

:  Astronomical  Collisions.     New  York,  1883.     8vo.     P. 

:  Observations  of  the  Transit  of  Venus,  1882.     New  Haven, 

1883.  8vo.     P. 

:  On  the  effect  of  flexure  of  the  Axis  in  Transit  instru- 
ments, etc.  Northfield,  1883.  8vo.  P. 

:  Spectroscopic  Notes.     New  Haven,  1883.     8vo.     P. 

:  Pending  Problems  in  Astronomy.    Salem,  1885.    8vo.    P. 

:  Physical  Constitution  of  the  Sun.  Philadelphia,  1885. 

8vo.  P. 

:  A  text-book  of  General  Astronomy.     Boston,  1888.     8vo. 

:  Description  of  detached  gravity  escapement.  Ms.  n.  p., 

n.  d.  4to.  P. 

:  Ten  Years'  Progress  in  Astronomy,  1876-86.  n.  p.,  n.  d. 

8vo.  P. 

:  The  recent  solar  eclipse  (1878)  (from  the  Princeton 

Review),  n.  d.  8vo.  P. 

:  Theories  regarding  the  Sun's  Corona.  New  York,  n.  d. 

8vo.  P. 

:  Practical  uses  of  electricity,     n.  p.,  n.  d.     8vo.     P. 

:  See  LANGLEY. 


Lick  Observatory  Library.  121* 

ZACH  (F.  X.  von):  Monatliche  Correspondenz.  Vols.  1/2,  3,  4, 
5,  6,  7,  8,  9,  10,  11,  12,  13,  14,  15,  16,  17,  18,  19,  20,  21,  22, 
23,  24,  25, 26,  27,  28.  Register  von  Dr.  J.  G.  GALLE.  (1850.) 
Gotha,  1800-13.  8vo. 

:  Correspondence  Astronomique,  Geographique,  Hydro- 

graphique  et  Statistique.  Vol.  I  (1818-19);  Vol.  II,  1819; 
Vol.  Ill,  1819;  Vol.  IV  (1820);  Vol.  V  (1821);  Vol.  VI 
(1822);  Vol.  VII  (1822);  Vol.  VIII  (1823);  Vol.  IX 
(1823);  Vol.  X  (1824);  Vol.  XI  (1824);  Vol.  XII  (1825); 
Vol.  XIII  (1825);  (Vol.  XIV-XV),  1826.  Genoa,  1818, 
1826-80. 

ZECH    (J.):    Tafeln    der    Additions    und    Subtractions    Loga- 

rithmen.     Leipzig,  1849.     8vo. 
:  Ueber  die  Mondfinsternisse  des  Almagest.     Leipzig,  1851. 

8vo.     P. 

ZEITSCHRIFT  FUR  ASTRONOMTE:  Von  LINDENAU  und  BOHNEN- 
BERGER.  Vols.  1,  2,  3,  4,  5,  6.  Tubingen,  1816-18.  8vo. 

'ZENGER  (C.  V.):  La  periode  solaire,etc.     Paris,  1887.     8vo.     P. 

:  La  duree  de  rotation  du  Soleil  comparie  a  celle  des 

planetes.  Paris,  1888.  8vo.  P. 

:  La  spectrophotographie  des  parties  invisibles  du  spectre 

solaire.  Paris,  1889.  4to.  P. 

:  Die  periodischen  Wettersturze  des  Erdenjahres,  etc. 

Magdeburg,  1889.  8vo.  P.* 

ZETTNOW  (E.)  and  SCHUMANN  (V.):  Ueber  Erythrosinsilber- 
platten  mit  Silberueberschuss.  (Leipzig),  (1889).  8vo. 

ZOELLNER  (J.  C.  F.):  Photometrische  Untersuchungen.  Leip- 
zig, 1865.  8vo. 


***  By  a  misunderstanding,  a  number  of  the  pages  of  the  preceding  Catalogue  were 
struck  off  before  revision  by  the  author,  and  a  few  material  errors  remain  in  the 
text,  which  the  reader  can,  however,  easily  correct  for  himself. 


WORKS  ISSUED  BY  THE  LICK  OBSERVATORY. 


1.  Publications  of  the  Lick  Observatory  of  the  University  of 

California,  prepared  under  the  direction  of  the  Lick 
Trustees  by  EDWARD  S.  HOLDEN.  Volume  1, 1887.  Sacra- 
mento, 1887.  4to. 

2.  Suggestions  for  Observing  the  Total  Eclipse  of  the  Sun  on 

January  1,  1889,  by  EDWARD  S.  HOLDEN.  Printed  by 
authority  of  the  Regents  of  the  University  of  California. 
Sacramento,  1888.  8vo. 

3.  Reports  on  the  Observations  of  the  Total  Eclipse  of  the  Sun 

of  January  1,  1889,  published  by  the  Lick  Observatory. 
Printed  by  authority  of  the  Regents  of  the  University  of 
California.  Sacramento,  1889.  8vo. 

4.  Reports  on  the  Observations  of  the  Total  Eclipse  of  the  Sun, 

December-  21-22,  1889,  and  of  the  Total  Eclipse  of  the 
Moon,  July  22,  1888,  to  which  is  added  a  Catalogue  of 
the  Library,  published  by  the  Lick  Observatory.  Printed 
by  authority  of  the  Regents  of  the  University  of  California. 
Sacramento,  1891.  8vo. 


14  DAY  USE 

RETURN  TO  DESK  FROM  WHICH  BORROWED 

LOAN  DEPT. 

This  book  is  due  on  the  last  date  stamped  below,  or 

on  the  date  to  which  renewed. 
Renewed  books  are  subject  to  immediate  recall. 


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THE  UNIVERSITY  OF  CALIFORNIA  LIBRARY 

